# Nuclear Physics in Astrophysics VIII

Europe/Rome
Sala conferenze (Laboratori Nazionali del Sud)

### Sala conferenze

#### Laboratori Nazionali del Sud

Via S. Sofia 62 I-95123 Catania Italy
,
Description
The 8th Nuclear Physics in Astrophysics International conference will be held from June 18th through June 23rd, 2017 in Catania, Italy.

NPA8 is supported by the European Physical Society

by the Istituto Nazionale di Fisica Nucleare

and by the Department of Physics and Astronomy of the University of Catania

We also acknowledge the support of:

Participants
• Alba Formicola
• Aleksandra Cvetinović
• Alessandro Alberto Oliva
• Alessia Francesca Di Pietro
• Alex Zylstra
• Alexander Solovyev
• Alisa Galishnikova
• Alison Laird
• Aliya Nurmukhanbetova
• Andre Sieverding
• Andreas Best
• Angelo Pagano
• Annamaria Muoio
• Annika Lennarz
• Anton Wallner
• Antti Saastamoinen
• Anu Kankainen
• Artemis Spyrou
• Aurora Tumino
• Axel Boeltzig
• Brian Fields
• Carlo Broggini
• Carlos Bertulani
• Carmen Altana
• Chiara Mazzocchi
• Chris Wrede
• Christoph Langer
• Claire Fullarton
• Claudio Spitaleri
• Clemens Wolf
• Daid Kahl
• Dan Cozma
• Daniel Bemmerer
• Daniele Dell'Aquila
• Daniyar Janseitov
• Diego Vescovi
• Dimiter Balabanski
• Dinara Valiolda
• Domingo Anibal Garcia-Hernandez
• Dosbol Nauruzbayev
• Efraín Chavez
• Elena Fedorova
• Emanuel Pollacco
• Emilio Andrea Maugeri
• Enrique Zas
• Fairouz Hammache
• Fausto Casaburo
• Felix Heim
• Francesca Romana Pantaleo
• François de Oliveira Santos
• Gabor Kiss
• Gabriel Martinez-Pinedo
• Gaetano Lanzalone
• Georgios Perdikakis
• Giovanni Francesco Ciani
• Giovanni Luca Guardo
• Giuseppe Cardella
• Giuseppe D'Agata
• Giuseppe Gabriele Rapisarda
• Giuseppe Verde
• Gwenaelle Gilardy
• György Gyürky
• Heinrich Wilsenach
• Hernan Quevedo
• Heshani Jayatissa
• Hidetoshi Yamaguchi
• Ivano Lombardo
• Jaromir Mrazek
• Jeffrey Blackmon
• Jenny Feige
• Jesús Casal
• Jolie Cizewski
• Jorge Horvath
• Jos Riley
• Laetitia Canete
• Laszlo Csedreki
• Livio Lamia
• Livius Marian Trache
• Luciano Calabretta
• LUIS ARMANDO ACOSTA SANCHEZ
• Magdalena Skurzok
• Marco La Cognata
• MARCO LIMONGI
• Maria Dorothea Schumann
• Maria Letizia Pumo
• Maria Letizia Sergi
• Marialuisa Aliotta
• Marisa Gulino
• Massimo Barbagallo
• Matej Lipoglavsek
• Matthew Williams
• Maurizio Maria Busso
• Michael Febbraro
• Mikhail Barabanov
• Moshe Gai
• Neven Soic
• Nicola Colonna
• Nicolas de Séréville
• Nicolas Hubbard
• Oliver Kirsebom
• Oliver Kirsebom
• Oscar Trippella
• Pavel Zarubin
• Peter Mohr
• Philipp Scholz
• Philippe CHOMAZ
• Pierpaolo Figuera
• Pierre Descouvemont
• Raffaele Buompane
• Ralitsa Ilieva
• Rebecca Surman
• Rene Reifarth
• Richard deBoer
• Roberta Sparta'
• Rosanna Depalo
• Rosario Gianluca Pizzone
• Ruchi Garg
• Ryan Wilkinson
• Salvatore Cavallaro
• Salvatore Messina
• Salvatore Tudisco
• Sandrine Courtin
• Sara Palmerini
• Sarah Stern
• Sebastiana Maria Puglia
• Seiya Hayakawa
• Silvio Cherubini
• Stefan Fiebiger
• Stefan Typel
• Stefano Romano
• Stephane Goriely
• Stephanie Lyons
• Svetlana Chesnevskaya
• Taka Kajino
• Tamás Szücs
• Tanja Heftrich
• Tatyana Belyaeva
• Teresa Kurtukian Nieto
• Toshio Suzuki
• Vaclav Burjan
• Viacheslav Samarin
• Viviana Mossa
• Vàclav Kroha
• Zsolt Fulop
• Sunday, 18 June
• 18:00 20:00
Welcome cocktail 2h Cappella Bonajuto

#### Cappella Bonajuto

Via Bonajuto 9/13 Catania
• Monday, 19 June
• 08:30 09:10

### Sala conferenze

#### Laboratori Nazionali del Sud

Via S. Sofia 62 I-95123 Catania Italy
• 09:10 11:20
Explosive nucleosynthesis observations Sala conferenze

### Sala conferenze

#### Laboratori Nazionali del Sud

Via S. Sofia 62 I-95123 Catania Italy
• 09:10
When Stars Attack! Live Radioisotopes Reveal Near-Earth Supernovae 30m
% % Nuclear Physics in Astrophysics 8 template for abstract % % Format: LaTeX2e. % % Rename this file to name.tex, where name' is the family name % of the first author, and edit it to produce your abstract. % \documentstyle[11pt]{article} % % PAGE LAYOUT: % \textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset -0.35in \topmargin 0.305in \oddsidemargin +0.35in \evensidemargin -0.35in \def\iso#1#2{\mbox{${}^{#2}{\rm #1}$}} \def\fe6#1{\iso{Fe}{6#1}} %\renewcommand{\rmdefault}{ptm} % to use Times font \long\def\TITLE#1{{\Large{\bf#1}}}\long\def\AUTHORS#1{ #1\\[3mm]} \long\def\AFFILIATION#1#2{$^{#1}\,$ #2\\} \begin{document} {\small \it Nuclear Physics in Astrophysics 8, NPA8: 18-23 June 2017, Catania, Italy} \vspace{12pt} \thispagestyle{empty} \begin{center} %%% %%% Title goes here. %%% \TITLE{When Stars Attack! \\ Live Radioisotopes Reveal Near-Earth Supernovae }\\[3mm] %%% %%% Authors and affiliations are next. The presenter should be %%% underlined as shown below. %%% \AUTHORS{Brian D. Fields$^{1,2}$} %%% {\small \it \AFFILIATION{1}{Department of Astronomy, University of Illinois} \AFFILIATION{2}{Department of Physics, University of Illinois} } %%% \vspace{12pt} % Do not modify % Enter contact e-mail address here. \centerline{Contact email: {\it bdfields@illinois.edu}} \vspace{18pt} % Do not modify \end{center} %%% %%% Abstract proper starts here. %%% Supernovae are major engines of nucleosynthesis, and create many of the elements essential for life. Yet these awesome events take a sinister shade when they occur close to home, because an explosion very nearby would pose a grave threat to Earthlings. We will show how radionuclides produced by supernovae can reveal nearby events in the geologic past, and we will highlight isotopes of interest. In particular, accelerator mass spectrometry has detected live \fe60 globally in deep-ocean material, and in lunar samples. We will review astrophysical \fe60 production sites and show that the data demand that one or more core-collapse supernovae exploded near the Earth $\sim ~3$ Myr ago, and explain how debris from the explosion was transported to the Earth as a radioactive rain.'' The \fe60 measurements represent a new tool for nuclear astrophysics: we can now use sea sediments and lunar cores as telescopes, probing supernova nucleosynthesis and possibly even indicating the direction towards the event(s). We will close by reviewing recent work showing that an explosion so close was probably a near-miss'' that exposed the biosphere to intense and possibly harmful ionizing radiation. %%[1,2]. \bigskip {\small %%\noindent [1] E. Stark, Phys. Journal of the North 83 045801 (2011); \noindent %%[2] O. Martell et al. submitted to Solar Physics Letters (2013).} %%% %%% End of abstract. %%% \end{document}
Speaker: Prof. Brian Fields (Departments of Astronomy and of Physics, University of Illinois)
• 09:40
60Fe and 244Pu in deep-sea archives - a link to nearby supernova activity and r–process sites 30m
% % Nuclear Physics in Astrophysics 8 template for abstract % % Format: LaTeX2e. % % Rename this file to name.tex, where name' is the family name % of the first author, and edit it to produce your abstract. % \documentstyle[11pt]{article} % % PAGE LAYOUT: % \textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset -0.35in \topmargin 0.305in \oddsidemargin +0.35in \evensidemargin -0.35in %\renewcommand{\rmdefault}{ptm} % to use Times font \long\def\TITLE#1{{\Large{\bf#1}}}\long\def\AUTHORS#1{ #1\\[3mm]} \long\def\AFFILIATION#1#2{$^{#1}\,$ #2\\} \begin{document} {\small \it Nuclear Physics in Astrophysics 8, NPA8: 18-23 June 2017, Catania, Italy} \vspace{12pt} \thispagestyle{empty} \begin{center} %%% %%% Title goes here. %%% \TITLE{$^{60}$Fe and $^{244}$Pu in deep-sea archives - a link to nearby supernova activity and r--process sites }\\[3mm] %%% %%% Authors and affiliations are next. The presenter should be %%% underlined as shown below. %%% \AUTHORS{A. Wallner$^{1}$, N. Kinoshita$^{2}$, J. Feige$^{3}$, M. Froehlich$^{1}$, M. Hotchkis$^{4}$, L.K. Fifield$^{1}$, R. Golser$^{5}$, M. Honda$^{6}$, U. Linnemann$^{7}$, H. Matsuzaki$^{8}$, S. Merchel$^{9}$, M. Paul$^{10}$, G. Rugel$^{9}$, D. Schumann$^{10}$, S.G. Tims$^{1}$, P. Steier$^{5}$, T. Yamagata$^{12}$, S.R. Winkler$^{5}$}. %%% {\small \it \AFFILIATION{1}{Department of Nuclear Physics, The Australian National University, ACT 2601, Australia} \AFFILIATION{2}{Institute of Technology, Shimizu Corporation, Tokyo 135-8530, Japan} \AFFILIATION{3}{Department of Astronomy and Astrophysics, Berlin Institute of Technology, Berlin, Germany} \AFFILIATION{4}{Australian Nuclear Science and Technology Organisation (ANSTO), Lucas Heights, Australia} \AFFILIATION{5}{University of Vienna, Faculty of Physics, Isotope Research, VERA Laboratory, Austria} \AFFILIATION{6}{Graduate School of Pure and Applied Sciences, University of Tsukuba, Japan} \AFFILIATION{7}{Senckenberg Collections of Natural History Dresden, GeoPlasmaLab, Dresden, Germany} \AFFILIATION{8}{MALT, The University of Tokyo, Tokyo, Japan} \AFFILIATION{9}{Helmholtz-Zentrum Dresden-Rossendorf (HZDR), Dresden, Germany} \AFFILIATION{10}{Racah Institute of Physics, The Hebrew University of Jerusalem, Jerusalem 91904, Israel} \AFFILIATION{11}{Biology and Chemistry, Paul Scherrer Institute (PSI), 5232 Villigen, Switzerland} \AFFILIATION{11}{Graduate School of Integrated Basic Sciences, Nihon University, Tokyo, Japan} } %%% \vspace{12pt} % Do not modify % Enter contact e-mail address here. \centerline{Contact email: {\it anton.wallner@anu.edu.au}} \vspace{18pt} % Do not modify \end{center} %%% %%% Abstract proper starts here. %%% The Interstellar Medium (ISM) is continuously fed with new nucleosynthetic products. The solar system moves through the ISM and collects dust particles. Therefore, direct detection of freshly produced radionuclides on Earth, i.e. before decaying, provide insight into recent and nearby nucleosynthetic activities [1,2]. Indeed, a pioneering work at TU Munich [3,4], which applied the ultra-sensitive single atom counting technique of accelerator mass spectrometry (AMS) to an ocean crust-sample, showed an enhanced $^{60}$Fe signal possibly of extraterrestrial origin. Within an international collaboration [5-7] we have continued to search for ISM radionuclides incorporated in terrestrial archives. We have analyzed several deep-sea sediments, crusts and nodules for extraterrestrial $^{60}$Fe (t$_{1/2}$=2.6 Myr), $^{26}$Al (t$_{1/2}$=0.7 Myr) and $^{244}$Pu (t$_{1/2}$=81 Myr) [5-8] which are complemented by independent work at TU Munich [9-11]. All the data demonstrate a clear global $^{60}$Fe influx that is interpreted as exposure of Earth to recent ($\le${10} Myr) supernova explosions. Furthermore, the low concentrations measured for $^{244}$Pu suggest an unexpectedly low abundance of interstellar $^{244}$Pu [5]. This finding signals a rarity of actinide r--process nucleosynthesis which is incompatible with the rate and expected yield of standard core collapse supernovae as the predominant actinide-producing sites. In this talk I will also present additional new results for $^{60}$Fe and $^{244}$Pu measured with unprecedented sensitivity. These data provide new insights into their concomitant influx and their ISM concentrations over a time period of the last 11 million years. \bigskip {\small [1] J. Ellis et al.,\emph{ ApJ.} \textbf{470}, 1227 (1996). [2] G. Korschinek et al.,\emph{ Radiocarbon} \textbf{38}, 68 (1996); abstract. [3] K. Knie et al.,\emph{ Phys. Rev. Lett.} \textbf{83}, 18 (1999). [4] K. Knie et al.,\emph{ Phys. Rev. Lett.} \textbf{93}, 171103 (2004). [5] A. Wallner et al.,\emph{ Nature Comm.} \textbf{6}, 5956 (2015). [6] J. Feige et al., \emph{EPJ Web of Conf.} \textbf{63}, 3003 (2013). [7] A. Wallner et al.,\emph{ Nature} \textbf{532}, 69 (2016). [8] M. Paul M. et al. \emph{Astrophys. J. Lett.} \textbf{558}, L133âL135 (2001). [9] C. Wallner et al. \emph{New Astron. Rev.} \textbf{48}, 145â150 (2004). [10] L. Fimiani et al.,\emph{ Phys. Rev. Lett.} \textbf{116}, 151104 (2016). [11] P. Ludwig et al.,\emph{ PNAS} \textbf{113}, 9232 (2016).} %%% %%% End of abstract. %%% \end{document}
Speaker: Prof. Anton Wallner (The Australian National University)
• 10:10
Recent Ultra High Energy neutrino bounds and multimessenger observations with the Pierre Auger Observatory 30m
The overall picture of the highest energy particles produced in the Universe is changing because of measurements made with the Pierre Auger Observatory. Composition studies point towards an unexpected mixed composition of intermediate mass nuclei, more isotropic than anticipated, which is reshaping the future of the field and underlining the priority to understand composition at the highest energies. The Observatory is competitive in the search for neutrinos of all flavours above about 100 PeV by looking for very inclined showers produced deep in the atmosphere by neutrinos interacting either in the atmosphere or in the Earth's crust and covering a declination field of view between $-65^\circ$ and $60^\circ$ in equatorial coordinates. ​​Neutrinos are produced in ultra high energy cosmic ray ​interactions and they provide valuable complementary information, their fluxes being sensitive to the primary cosmic ray masses and their directions reflecting the source positions. We report the results of the neutrino search providing competitive bounds to neutrino production and strong constraints to a number of production models including cosmogenic neutrinos due to ultra high energy protons. We also report on two recent contributions of the Observatory to multimessenger studies​.​ The correlations of the directions of the highest energy astrophysical neutrinos discovered with IceCube ​and​ the highest energy cosmic rays detected with the Auger Observatory and the Telescope Array​,​ and the targeted search for neutrinos correlated with the discovery of the gravitational​-​wave events GW150914 and GW151226 ​discovered ​with ​​advanced LIGO.
Speaker: Prof. Enrique Zas (IGFAE - University of Santiago)
• 10:40
Limits on $^{60}$Fe/$^{26}$Al nucleosynthesis ratios from deep-sea sediment AMS measurements 20m
% % Nuclear Physics in Astrophysics 8 template for abstract % % Format: LaTeX2e. % % Rename this file to name.tex, where name' is the family name % of the first author, and edit it to produce your abstract. % \documentstyle[11pt]{article} % % PAGE LAYOUT: % \textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset -0.35in \topmargin 0.305in \oddsidemargin +0.35in \evensidemargin -0.35in %\renewcommand{\rmdefault}{ptm} % to use Times font \long\def\TITLE#1{{\Large{\bf#1}}}\long\def\AUTHORS#1{ #1\\[3mm]} \long\def\AFFILIATION#1#2{$^{#1}\,$ #2\\} \begin{document} {\small \it Nuclear Physics in Astrophysics 8, NPA8: 18-23 June 2017, Catania, Italy} \vspace{12pt} \thispagestyle{empty} \begin{center} %%% %%% Title goes here. %%% \TITLE{Limits on $^{60}$Fe/$^{26}$Al nucleosynthesis ratios from deep-sea sediment AMS measurements}\\[3mm] %%% %%% Authors and affiliations are next. The presenter should be %%% underlined as shown below. %%% \AUTHORS{J. Feige$^{1,2}$, A. Wallner$^{2,3}$, L.~K. Fifield$^3$, R. Golser$^2$, S. Merchel$^4$, G. Rugel$^4$, P. Steier$^2$,\\ S.~G. Tims$^3$, S.~R. Winkler$^{2,5}$} %%% {\small \it \AFFILIATION{1}{Department of Astronomy and Astrophysics, Berlin Institute of Technology, Berlin, Germany} \AFFILIATION{2}{University of Vienna, Faculty of Physics - Isotope Research and Nuclear Physics, Vienna, Austria} \AFFILIATION{3}{Department of Nuclear Physics, The Australian National University, Canberra, Australia} \AFFILIATION{4}{Helmholtz-Zentrum Dresden-Rossendorf, Dresden, Germany} \AFFILIATION{5}{iThemba LABS, Somerset West, South Africa} } %%% \vspace{12pt} % Do not modify % Enter contact e-mail address here. \centerline{Contact email: {\it feige@astro.physik.tu-berlin.de}} \vspace{18pt} % Do not modify \end{center} %%% %%% Abstract proper starts here. %%% The long-lived radionuclide $^{26}$Al (t$_{1/2}$\,=\,0.7\,Myr) has been observed throughout our galaxy, reflecting ongoing nucleosynthesis over the past few million years [1]. It is produced and ejected into the interstellar medium by stellar winds and during supernova explosions. A nearby supernova may leave an imprint of $^{26}$Al in terrestrial archives, complementing the observation of supernova-produced $^{60}$Fe in deep-sea samples. \\ The same set of sediment samples from the Indian Ocean that showed a distinct $^{60}$Fe-signature in layers of ages between 1.7 and 3.2\,Myr [2] was also analyzed for $^{26}$Al. However, additional terrestrial sources producing $^{26}$Al on Earth, such as cosmogenic production in the atmosphere and in-situ production within the sediment, may obscure a supernova imprint. \\ We used our experimental $^{26}$Al data to infer lower limits on $^{60}$Fe/$^{26}$Al nucleosynthesis ratios by comparing the width and the strength of the previously measured $^{60}$Fe-signal to our $^{26}$Al data. We find that our results generally favour the higher theoretical isotopic supernova ratios and deviate from the observed galactic $^{60}$Fe/$^{26}$Al flux ratio by 2-3 times of the measurement uncertainty. \bigskip {\small \noindent [1] Diehl et al., New Astron. Rev., 52, 440 (2008); \noindent [2] Wallner, Feige et al., Nature, 532, 69 (2016).} %%% %%% End of abstract. %%% \end{document}
Speaker: Dr Jenny Feige (Berlin Institute of Technology)
• 11:20 11:40
Coffee break 20m Sala conferenze

### Sala conferenze

#### Laboratori Nazionali del Sud

Via S. Sofia 62 I-95123 Catania Italy
• 11:40 13:20
r-process 1 Sala conferenze

### Sala conferenze

#### Laboratori Nazionali del Sud

Via S. Sofia 62 I-95123 Catania Italy
• 11:40
Explosive nucleosynthesis of heavy elements: an astrophysical and nuclear physics challenge 30m
Half of the elements heavier than iron are produced by the r process under extreme conditions. To identify its site remains one of the major challenges in nuclear astrophysics. Advances in the description of neutrino-matter interactions and its implementation in core-collapse super- nova modelling have lead to the conclusion that supernova explosions only contribute to the production of elements with Z < 50. Compact binary mergers are currently considered the best candidate for the main r-process site. These events are expected to produce gravitational waves, likely to be observed by the LIGO collaboration, and eject large amounts of neutron-rich mate- rial where the r process operates. In this talk, I will discuss the important role of nuclear physics to determine the r-process yields from compact binary mergers. In addition to neutron captures and beta decay, fission rates and yields of superheavy neutron-rich nuclei are fundamental to un- derstand the r-process dynamics and nucleosynthesis. Mergers constitute also ideal candidates to directly observe the r-process via an electromagnetic transient due to the radioactive decay of r-process material. This type of event, known as kilonova, may have already been observed associated with the gamma-ray burst GRB 130603B.
Speaker: Prof. Gabriel Martínez Pinedo (Technische Universität Darmstadt)
• 12:10
Solving the mystery of r-process: mergers vs. supernovae 30m
Taka Kajino, Shota Shibagaki, Yutaka Hirai, Grant J. Mathews The origin of heavy elements heavier than iron like Au and U are still unknown although sixty years have already passed since the benchmark paper B2FH on the origin of elements in the Universe was published in 1957. GW emitters of both binary neutron-star mergers (NSMs) and core-collapse supernovae (SNe) are viable candidates for the production site of heavy elements called r-process elements. SN models of magneto-rotationally driven jets (MHD-Jet SNe) naturally explain the ”universality” in the observed abundance pattern between the solar- system and extremely metal-poor stars in the Milky Way halo or recently discovered ultra-faint dwarf galaxies. However, full understanding of their explosion mechanism is still in progress. NSM models, on the other hand, have a serious difficulty that their arrival is delayed due to very slow GW radiation at least 100 My (”time-scale problem”), which could not contribute to the early galaxies. We will first discuss that our high-resolution N-body/SPH simulation of Galactic chemo-dynamical evolution solve this ”time-scale problem” partially, leaving a serious discrepancy in the early Galactic evolution [1,2]. We will then propose a new theoretical model such that the MHD-Jet SNe first contribute to the enrichment of heavy elements in the early galaxies, then the NSMs follow gradually towards the solar system [3-5]. Our new model satisfies the ”universality” and predicts several specific observational evidences for the time evolution of isotopic abundance pattern [5]. [1] Y. Hirai, Y. Ishimaru, T. R. Saitoh, M. S. Fujii, J. Hidaka, and T. Kajino, ApJ 814 (2015), 4. [2] Y. Hirai, Y. Ishimaru, T. R. Saitoh, M. S. Fujii, J. Hidaka, and T. Kajino, MNRAS 466 (2017) 2472. [3] S. Shibagaki, T. Kajino, G. J. Mathews, S. Chiba, S. Nishimura, and G. Lorusso, ApJ 816 (2016) 79. [4] S. Shibagaki, et al. (2017) to be submitted. [5] T. Kajino, and G. J. Mathews, Rep. Prog. Phys. (2017) in press.
Speaker: Prof. Taka Kajino (NAOJ, The University of Tokyo)
• 12:40
The neutrino process in supernova nucleosynthesis 20m
Speaker: Mr Andre Sieverding (Technische Universität Darmstadt)
• 13:00
Roles of nuclear weak rates on the evolution of degenerate cores in stars 20m
% % Nuclear Physics in Astrophysics 8 template for abstract % % Format: LaTeX2e. % % Rename this file to name.tex, where name' is the family name % of the first author, and edit it to produce your abstract. % \documentstyle[11pt]{article} % % PAGE LAYOUT: % \textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset -0.35in \topmargin 0.305in \oddsidemargin +0.35in \evensidemargin -0.35in %\renewcommand{\rmdefault}{ptm} % to use Times font \long\def\TITLE#1{{\Large{\bf#1}}}\long\def\AUTHORS#1{ #1\\[3mm]} \long\def\AFFILIATION#1#2{$^{#1}\,$ #2\\} \begin{document} {\small \it Nuclear Physics in Astrophysics 8, NPA8: 18-23 June 2017, Catania, Italy} \vspace{12pt} \thispagestyle{empty} \begin{center} %%% %%% Title goes here. %%% \TITLE{Roles of nuclear weak rates on the evolution of degenerate cores in stars}\\[3mm] %%% %%% Authors and affiliations are next. The presenter should be %%% underlined as shown below. %%% \AUTHORS{ Toshio Suzuki$^{1,2}$, N. Tsunoda$^{3}$, Y. Tsunoda$^{3}$, N. Shimizu$^{3}$, T. Otsuka$^{4,5}$} %%% {\small \it \AFFILIATION{1}{Department of Physics, College of Humanities and Sciences, Nihon University, Setagaya-ku, Tokyo 156-8550, Japan} \AFFILIATION{2}{National Astronomical Observatory of Japan, Mitaka, Tokyo 181-8588, Japan} \AFFILIATION{3}{Center for Nuclear Study, The University of Tokyo, Hongo, Tokyo 113-0033, Japan} \AFFILIATION{4}{Department of Physics, The University of Tokyo, Hongo, Tokyo 113-0033, Japan} \AFFILIATION{5}{National Superconducting Cyclotron Laboratory, Michigan State University, %East Lansing, MI 48824, USA} } %%% \vspace{12pt} % Do not modify % Enter contact e-mail address here. \centerline{Contact email: {\it suzuki@phys.chs.nihon-u.ac.jp}} \vspace{18pt} % Do not modify \end{center} %%% %%% Abstract proper starts here. %%% Electron-capture and $\beta$-decay rates in nuclei at stellar environments evaluated with new shell-model Hamiltonians have been applied to cooling processes and nucleosynthesis in electron-degenerate cores in stars. Nuclear Urca processes in electron-degenerate O-Ne-Mg cores of stars with initial masses of 8-10 M$_{\odot}$ have been studied using the weak rates for $sd$-shell nuclei obtained for the USDB Hamiltonian, and the processes for nuclear pairs with A=23 and 25 are found to be important for the cooling of the cores and determination of the final fate of the stars [1]. Important roles of the nuclear Urca processes have been pointed out also in C-O and hybrid C-O-Ne white dwarfs (WD) [2,3]. The nuclear weak rates obtained in a large region of $pf$-shell nuclei by GXPF1J [4] have been applied to study nucleosynthesis in Type-Ia supernova explosions (SNe), which result from accreting C-O WD in close binaries. Over-production of neutron-rich isotopes in the iron group elements compared to the solar abundance noticed for the Fuller-Fowler-Newman rates has been considerably reduced [5]. We extend our study of applications of updated nuclear weak rates to cooling processes and evolution of degenerate cores in stars in the region outside one-major $sd$- and $pf$-shells. The weak rates for nuclear pairs important for Urca processes in neutron star crusts [6] are studied. In particular, weak rates of nuclei in the island of inversion such as $^{31}$Mg are evaluated based on microscopic interactions obtained by extended Kuo-Krenciglowa (EKK) method [7]. The method can explain well the structure of neutron-rich Mg isotopes. Spectra of $^{31}$Mg, in particular, are successfully reproduced by the EKK method in contrast to other approaches. Fe-core-collapse SNe are sensitive to the e-capture rates for extremely neutron-rich isotopes near $^{78}$Ni [8] as well as iron group nuclei. Electron-capture rates in $^{78}$Ni are evaluated with extension of the configuration space outside the $pf$-shell [9], and compared with RPA calculations and Sullivan’s approximate formula [8]. In $p$-shell region, an accurate shell-model evaluation is carried out for e-capture rates on $^{13}$N, which is important during carbon simmering stage of C-O WD prior to the onset of thermonuclear explosions [3]. Nuclear weak transition rates, thus, play important roles on the final evolution of degenerate cores in stars. Accurate evaluation of the nuclear weak rates is essential for the studies of astrophysical processes sensitive to the rates. \bigskip {\small \noindent [1] T. Suzuki, H. Toki and K. Nomoto, ApJ. 817 (2016) 163; H. Toki, T. Suzuki, K. Nomoto, S. Jones and R. Hirsci, Phys. Rev. C 88 (2013) 015806; S. Jones et al., ApJ. 772 (2013) 150. \noindent [2] P. A. Dennisenkov et al., MNRAS 447 (2015) 2696. \noindent [3] H. Martinez-Rodriguez et al., ApJ. 825 82016) 57. \noindent [4] M. Honma et al., Phy. Rev. C 69 (2004) 034335; J. Phys. Conf. Ser. 20 (2005) 7. \noindent [5] K. Mori, M. A. Famiano, T. Kajino, T. Suzuki et al., %, J. Hidaka, M. Honma, K. Iwamoto, K. Nomoto and T. Otsuka, ApJ. 833 (2016) 179. \noindent [6] H. Schatz et al., Nature 505 (2014) 62. \noindent [7] N. Tsunoda, T. Otsuka, K.Shimizu, M. Hjorth-Jensen, K, Takayanagi and T. Suzuki, Phys. Rev. C (2017) to be published. \noindent [8] C. Sullivan et al., ApJ. 816 (2016) 44. \noindent [9] Y. Tsunoda et al, Phys. Rev. C 89 (2014) 031301(R).} %%% %%% End of abstract. %%% \end{document}
Speaker: Prof. Toshio Suzuki (Nihon University)
• 13:30 14:30
Lunch 1h Sala conferenze

### Sala conferenze

#### Laboratori Nazionali del Sud

Via S. Sofia 62 I-95123 Catania Italy
• 14:30 16:00
r-process 2 Sala conferenze

### Sala conferenze

#### Laboratori Nazionali del Sud

Via S. Sofia 62 I-95123 Catania Italy
• 14:30
The r-process nucleosynthesis and related nuclear challenges 30m
The r-process nucleosynthesis and related nuclear challenges S. Goriely Institut d’Astronomie et d’Astrophysique, Université Libre de Bruxelles, Belgium Contact email: sgoriely@astro.ulb.ac.be The rapid neutron-capture process, or r-process, is known to be of fundamental importance for explaining the origin of approximately half of the A > 60 stable nuclei observed in nature. In recent years nuclear astrophysicists have developed more and more sophisticated r-process models, eagerly trying to add new astrophysical or nuclear physics ingredients to explain the solar system composition in a satisfactory way. Recently, special attention has been paid to neutron star (NS) mergers following the confirmation by hydrodynamic simulations that a non- negligible amount of matter can be ejected and by nucleosynthesis calculations combined with the predicted astrophysical event rate that such events can account for the majority of r-material in our Galaxy We show here that the combined contribution of both the dynamical (prompt) ejecta expelled during binary NS or NS-black hole (BH) mergers and the neutrino and viscously driven outflows generated during the post-merger remnant evolution of relic BH-torus systems can lead to the production of r-process elements from mass number A >∼ 90 up to thorium and uranium. The corresponding abundance distribution is found to reproduce the solar distribution extremely well and can also account for the elemental distributions observed in low-metallicity stars. However, major uncertainties still affect our understanding of the composition of the matter ejected. These concern (i) the β-interactions of electron neutrinos and electron antineutrinos with free neutrons and protons, as well as their inverse reactions, which may affect the neutron-richness of the matter at the early phase of the ejection, and (ii) the nuclear physics of exotic neutron-rich nuclei, including nuclear structure as well as nuclear interaction properties, which impact the calculated abundance distribution resulting from the r-process nucleosynthesis. Both aspects will be critically discussed in the light of recent hydrodynamical simulations of NS mergers and microscopic calculations of nuclear decay and reaction probabilities.
Speaker: Stephane Goriely (Universite Libre de Bruxelles)
• 15:00
(file)
Speaker: Dr Jesús Casal (ECT*)
• 15:20
Effect of uncertainties in the statistical model description of n,$\gamma$ reactions to r-process nucleosynthesis 20m
% % Nuclear Physics in Astrophysics 8 template for abstract % % Format: LaTeX2e. % % Rename this file to name.tex, where name' is the family name % of the first author, and edit it to produce your abstract. % \documentstyle[11pt]{article} % % PAGE LAYOUT: % \textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset -0.35in \topmargin 0.305in \oddsidemargin +0.35in \evensidemargin -0.35in %\renewcommand{\rmdefault}{ptm} % to use Times font \long\def\TITLE#1{{\Large{\bf#1}}}\long\def\AUTHORS#1{ #1\\[3mm]} \long\def\AFFILIATION#1#2{$^{#1}\,$ #2\\} \begin{document} {\small \it Nuclear Physics in Astrophysics 8, NPA8: 18-23 June 2017, Catania, Italy} \vspace{12pt} \thispagestyle{empty} \begin{center} %%% %%% Title goes here. %%% \TITLE{Effect of uncertainties in the statistical model description of n,$\gamma$ reactions to r-process nucleosynthesis }\\[3mm] %%% %%% Authors and affiliations are next. The presenter should be %%% underlined as shown below. %%% \AUTHORS{\underline{G. Perdikakis}$^{1,2,4}$, S. Nikas$^{1,4}$, R. Surman$^{3,4}$, M. Beard$^{3, 4}$, M. Mumpower $^{5}$} %%% {\small \it \AFFILIATION{1}{Central Michigan University, Mt. Pleasant, MI 48859, USA} \AFFILIATION{2}{National Superconducting Cyclotron Laboratory, East Lansing, MI 48824, USA} \AFFILIATION{3}{University of Notre Dame, Notre Dame, IN 46556, USA} \AFFILIATION{4}{Joint Institute for Nuclear Astrophysics - Center for the Evolution of the Elements, East Lansing, MI 48824, USA} \AFFILIATION{5}{Los Alamos National Laboratory, Los Alamos, NM 87545, USA} } %%% \vspace{12pt} % Do not modify % Enter contact e-mail address here. \centerline{Contact email: {\it perdi1g@cmich.edu}} \vspace{18pt} % Do not modify \end{center} %%% %%% Abstract proper starts here. %%% While the role of the r-process in the synthesis of elements heavier than Iron is well established, the puzzling question of the actual astrophysical environment in which the process takes place still persists. In the current multi-messenger era, a multitude of observational information offers exciting opportunities to piece together an answer. Such efforts may depend critically in our ability to reproduce in nucleosynthesis calculations intricate features of the r-process abundance yield pattern (such as the location and height of the rare-earth peak, for example) in order to evaluate the feasibility of various nucleosynthesis scenarios. For such comparisons to be meaningful, however, uncertainties in the nuclear input that affect nucleosynthesis calculations have to be identified and evaluated. In this work, we study the effect of level density and gamma ray strength function modelling uncertainties to neutron capture reaction rates relevant for the r-process. The uncertainty observed in these reaction rates is also propagated to r-process abundance yields through reaction network calculations. %\bigskip %{\small % %\noindent [1] E. Stark, Phys. Journal of the North 83 045801 (2011); % %\noindent %[2] O. Martell et al. submitted to Solar Physics Letters (2013).} %%% %%% End of abstract. %%% \end{document}
Speaker: Georgios Perdikakis (Central Michigan University)
• 15:40
Constraining the rp-process by measuring $^{23}$Al(d,n)$^{24}$Si with GRETINA and LENDA at NSCL 20m
The $^{23}$Al(p,$\gamma$)$^{24}$Si stellar reaction rate has a significant impact of the light-curve emitted in X-ray bursts. Theoretical calculation shows that the reaction rate is mainly determined by the properties of direct capture as well as low-lying 2$^{+}$ states and a possible 4$^{+}$ state in $^{24}$Si. Currently, there is little experimental information on the properties of these states. We present a new experimental study, using surrogate reaction $^{23}$Al(d,n) at 47 AMeV at the National Superconducting Cyclotron Laboratory (NSCL),USA. We detect the full kinematics of the reaction, using the Gamma-Ray Energy Tracking In-beam Nuclear Array (GRETINA) to detect the $\gamma$-rays following the de-excitation of the reaction products, the Low Energy Neutron Detector Array (LENDA) to detect the recoiling neutrons and the S800 for identification of the $^{24}$Si recoils. These information will be used to determine the highly needed properties of the $^{24}$Si. \\ This work benefited from support by the National Science Foundation under Grant No. PHY-1430152 (JINA Center for the Evolution of the Elements). The research leading to these results has received funding from the European Research Council under the European Unions's Seventh Framework Programme (FP/2007-2013) / ERC Grant Agreement n. 615126. GRETINA was funded by the DOE, Office of Science. Operation of the array at NSCL was supported by DOE under Grant No. DE-SC0014537 (NSCL) and DE-AC02-05CH11231 (LBNL). This work were supported in part by the National Science foundation under Contract No. PHY-1102511.
Speaker: Clemens Wolf (Goethe-University Frankfurt)
• 16:00 16:30
Coffee break 30m Sala conferenze

### Sala conferenze

#### Laboratori Nazionali del Sud

Via S. Sofia 62 I-95123 Catania Italy
• 16:30 19:10
Direct measurements 1 Sala conferenze

### Sala conferenze

#### Laboratori Nazionali del Sud

Via S. Sofia 62 I-95123 Catania Italy
• 16:30
EXPERIMENTAL CHALLENGES IN UNDERGROUND NUCLEAR ASTROPHYSICS LABORATORY: PRESENT STATUS AND FUTURE OPPORTUNITIES 30m
Accurate knowledge of thermonuclear reaction rates is important in understanding energy generation, neutrino luminosity and nucleosynthesis in stellar interiors. Natural and Cosmic-ray-induced background can seriously limit the determination of reaction cross-sections at relevant energies for astrophysics. In order to improve the signal-to-noise ratio special care in experimental setups arrangement must be considered. In this talk I will review the experimental techniques adopted in underground nuclear astrophysics, giving an update of main results obtained, which shed lights on several key nuclear reactions that take place in various astrophysical scenarios. Moreover, I will give an overview of worldwide facilities, discussing the status and perspectives of the experiments which are running from several years or are in constructions or in early stage of development. I will, in particular, show their major scientific drivers, which will clearly lead to significant progress in answering many open questions in nuclear astrophysics
Speaker: Dr Alba Formicola (LNGS)
• 17:00
Catalysis of Nuclear Reactions by Electrons 30m
Electron screening enhances nuclear reaction cross sections at low beam energies. This happens in many astrophysical scenarios, e.g. stellar burning or supernova explosions. Unfortunately, the process is still poorly understood. All currently used calculations are based on the very simple assumption that the electrons distributed evenly on a shell decrease the repulsive potential inside the shell by a constant. Although the measurements in principle obey the predicted functional behavior of electron screening, its magnitude is severely underestimated by the theory. I will overview the current experimental situation and propose an alternative understanding of the electron screening process with a possible proof of its validity.
Speaker: Dr Matej Lipoglavsek (Jozef Stefan Institute, Ljubljana, Slovenia)
• 17:30
Direct study of the $^{22}$Ne({\it p,$\gamma$})$^{23}$Na reaction in inverse kinematics at DRAGON 20m
Speaker: Dr Annika Lennarz (TRIUMF)
• 17:50
First results of total and partial cross-section measurements of the 107Ag(p, $\gamma$)108Cd reaction 20m
The $\gamma$ process is assumed to play an important role in the nucleosynthesis of the majority of the p nuclei. Since the network of the $\gamma$ process includes so many different reactions and - mainly unstable - nuclei, cross-section values are predominantly calculated in the scope of the Hauser- Feshbach statistical model. The values heavily depend on the nuclear physics input-parameters. The results of total and partial cross-section measurements are used to improve the accuracy of the theoretical calculations. In order to extend the experimental database the 107Ag(p,$\gamma$)108Cd reaction was studied via the in-beam method at the high-efficiency HPGe $\gamma$-ray spectrometer HORUS at the University of Cologne. Proton beams with energies between 3.5 and 5.0 MeV were provided by the 10 MV FN-Tandem accelerator. First results on total and partial cross sections will be presented. Supported by the DFG (ZI 510/8-1) and the "ULDETIS" project within the UoC Excellence Initiative institutional strategy. P.S. and J.M. are supported by the Bonn-Cologne Graduate School of Physics and Astronomy.
Speaker: Mr Felix Heim (Institute for Nuclear Physics, University of Cologne)
• 18:10
Direct cross section measurement for the O-18(p,gamma)F-19 reaction at LUNA 20m
% % Nuclear Physics in Astrophysics 8 template for abstract % % Format: LaTeX2e. % % Rename this file to name.tex, where name' is the family name % of the first author, and edit it to produce your abstract. % \documentstyle[11pt]{article} % % PAGE LAYOUT: % \textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset -0.35in \topmargin 0.305in \oddsidemargin +0.35in \evensidemargin -0.35in %\renewcommand{\rmdefault}{ptm} % to use Times font \long\def\TITLE#1{{\Large{\bf#1}}}\long\def\AUTHORS#1{ #1\\[3mm]} \long\def\AFFILIATION#1#2{$^{#1}\,$ #2\\} \begin{document} {\small \it Nuclear Physics in Astrophysics 8, NPA8: 18-23 June 2017, Catania, Italy} \vspace{12pt} \thispagestyle{empty} \begin{center} %%% %%% Title goes here. %%% \TITLE{Direct cross section measurement for the $^{18}O(p,\gamma)^{19}F$ reaction at LUNA }\\[3mm] %%% %%% Authors and affiliations are next. The presenter should be %%% underlined as shown below. %%% \AUTHORS{F. R. Pantaleo$^{1,2}$, A. Best$^{3,4}$, G. Imbriani$^{3,4}$, R. Perrino$^2$ \par for the LUNA Collaboration} %%% {\small \it \AFFILIATION{1}{Universita' degli Studi di Bari, Dipartimento Interateneo di Fisica ''M. Merlin'', Bari, IT} \AFFILIATION{2}{INFN Bari, IT} \AFFILIATION{3}{Universita' degli Studi di Napoli, Dipartimento di Fisica "E. Pancini", Napoli, IT} \AFFILIATION{4}{INFN Napoli, IT} } %%% \vspace{12pt} % Do not modify % Enter contact e-mail address here. \centerline{Contact email: {\it francesca.pantaleo@ba.infn.it}} \vspace{18pt} % Do not modify \end{center} %%% %%% Abstract proper starts here. %%% The reaction $^{18}O(p,\gamma)^{19}F$ plays an important role in the context of Asymptotic Giant Branch (AGB) star evolution and nucleosynthesis. This reaction represents the bridge between CNO and other cycles, which are active during shell H burning. Moreover, the observed O isotope abundance in meteorites crucially depends on the precise knowledge of this rate at low energies. The low energy cross section of this reaction is influenced by the tails of higher energy broad states and by the presence of a state at 95 keV, which lies directly inside the energy window corresponding to the relevant stellar temperature range. \\In the context of the LUNA experiment we measured the low-energy cross section of this reaction, taking advantage of the low environmental background at the Gran Sasso underground laboratory. Two setups were used for the experimental campaign: measurements for the determination of the strength of the 95 keV resonance, disputed as predicted by [1,2], were done using a high-efficiency 4$\pi$ BGO detector, whereas gamma-ray branching measurements of the non-resonant low energy component and of higher-energy resonances utilized a high-resolution HPGe detector. The data taking has been concluded. The current status of the analysis will be presented. \bigskip {\small \\ \noindent[1] M. Q. Buckner et al. Phys. Rev. C 86, 065804 (2012) \\ \noindent [2] H.T. Fortune et al. Phys. Rev. C 015801 (2013) } %%% %%% End of abstract. %%% \end{document}
Speaker: Francesca Romana Pantaleo (Universita' degli Studi di Bari, Dipartimento Interateneo di Fisica ''M. Merlin'', Bari, IT, INFN Bari,Bari, IT)
• 18:30
Absolute measurement of the 7Be(p,g)8B cross section with the recoil separator ERNA 20m
7Be(p,g)8B still represents one of the major uncertainties on the predicted high energy component of solar neutrino flux and it has also a direct impact on the 7Li abundance after the Big Bang Nucleosynthesis. Previous experiments producing data with useful precision were performed in direct kinematics, using an intense proton beam on a radioactive 7Be target. The complicated target stoichiometry and the deterioration under beam bombardment might possibly be the origin of the discrepancies observed between the results of different measurements. Inverse kinematics, i.e. a 7Be ion beam and a hydrogen target, would shed light on systematic effects. Unfortunately, efforts attempted so far were limited by the low 7Be beam intensity. We present here a new experiment, exploiting a high intensity 7Be beam in combination with a windowless gas target and the recoil mass separator ERNA (European Recoil mass separator for Nuclear Astrophysics) at CIRCE (Center for Isotopic Research on Cultural and Environmental heritage), Caserta, Italy. Aim of the experiment is the measurement of the total reaction cross section by means of the direct detection of the 8B recoils. The experimental setup as well as results and their astrophysical impact will be illustrated.
Speaker: Raffaele Buompane (NA)
• 18:50
Production and characterization of 7Be targets for neutron cross section measurements 20m
Speaker: Prof. J.E. Horvath (IAG-USP, Sao Paulo, Brazil)
• 19:30
High-precision mass measurements for the rp-process at JYFLTRAP 2h
% Format: LaTeX2e. % % canete.tex % % \documentstyle[11pt]{article} \textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset -0.35in \topmargin 0.305in \oddsidemargin +0.35in \evensidemargin -0.35in \long\def\TITLE#1{{\Large{\bf#1}}}\long\def\AUTHORS#1{ #1\\[3mm]} \long\def\AFFILIATION#1#2{$^{#1}\,$ #2\\} \begin{document} {\small \it Nuclear Physics in Astrophysics 8, NPA8: 18-23 June 2017, Catania, Italy} \vspace{12pt} \thispagestyle{empty} \begin{center} \TITLE{High-precision mass measurements for the $rp$-process at JYFLTRAP}\\[3mm] \AUTHORS{L. Canete$^{1}$, T. Eronen$^{1}$, A. Jokinen$^{1}$, A. Kankainen$^{1}$, I.D. Moore$^{1}$, D. Nesterenko$^{1}$, S. Rinta-Antila$^{1}$, and the IGISOL group} %%% {\small \it \AFFILIATION{1}{University of Jyv\"{a}skyl\"{a}, P.O. Box 35 (YFL) FI-40014 University of Jyv\"{a}skyl\"{a}, Finland} } %%% \vspace{12pt} % Do not modify \centerline{Contact email: {\it lacanete@student.jyu.fi}} \vspace{18pt} % Do not modify \end{center} The rapid proton capture process ($rp$) is an important reaction network that generates nuclear energy and heavier elements via rapid hydrogen burning at high temperatures [1]. The $rp$-process occurs e.g. in type I X-ray bursts (XRB) which consists of a neutron star coupled to a low-mass main sequence star. The gravitational accretion of hydrogen and helium rich material from the companion star highly increases the temperature and the density at the surface of the neutron star and eventually causes a breakout from the hot CNO cycle [2]. The resulting $rp$-process shows a waiting point at $^{30}$S for most of the nucleosynthesis flow. The continuation of the network is then fully dependent of the ratio between four processes: the $\beta^+$-decay of $^{30}$S, the $^{30}$S($\alpha,p$)$^{33}$Cl reaction, the proton capture on $^{30}$S, and the photodisintegration of $^{31}$Cl. At typical XRB temperatures, the process is limitated by the long $\beta^+$-decay half-life of $^{30}$S ($T_{1/2}=1.178(5) s$) and the ratio between the proton captures on $^{30}$S and photodisintegration of $^{31}$Cl, which depends exponentially on the proton capture Q value i.e. on the masses of $^{31}$Cl and $^{30}$S. A better knowledge of the conditions where $^{30}$S acts as a waiting point is also valuable in observational astrophysics as double peaks in XRB bolometrical luminosity curve have been proposed to be explained by the $^{30}$S waiting point [3]. The JYFLTRAP double-Penning trap mass spectrometer at the IGISOL facility [4,5] has been successfully used to measure the mass of $^{31}$Cl with high precision [6]. The new mass value, $−7034.7(34)$keV, is 15 times more precise than the value given in the Atomic Mass Evaluation 2012 [7]. The first trap called the purification trap, is filled with helium gas and is used to cool the ions and remove the contaminants. The second trap, the precision trap, is used for mass measurements via time-of-flight ion cyclotron resonance (TOF-ICR) technique [8]. The recent results from JYFLTRAP and their impact on the $rp$-process will be discussed in this contribution. \bigskip {\small \noindent [1] R.K. Wallace and S.E. Woosley, Astrophys. J. Suppl. Ser. 45, 389 (1981); \noindent [2] A. Parikh and al., Prog. Part. Nucl. Phys. 69, 225-253 (2013); \noindent [3] J. L. Fisker and al., Astrophys. J. 608, L61 (2004); \noindent [4] T. Eronen et al., Eur. Phys. J. A 48, 46 (2012); \noindent [5] I. Moore et al., Nucl. Instrum. Methods Phys. Res., Sect. B 317, 208 (2013); \noindent [6] A. Kankainen et al., Phys. Rev. C 93, 041304(R) (2016); \noindent [7] M. Wang et al., Chin. Phys. C 36, 1603 (2012); \noindent [8] M. K\"{o}nig et al., Int. J. Mass Spectrom. Ion Processes 142, 95 (1995).} \end{document}
Speaker: Ms Laetitia Canete (University of Jyväskylä)
• 19:30
Introduction of the new LUNA experimental setup for high precision measurement of 13C(α,n)16O reaction for astrophysical purposes 2h
Nuclear Physics in Astrophysics 8, NPA8: 18-23 June 2017, Catania, Italy Introduction of the new LUNA experimental setup for high precision measurement of 13C(α,n)16O reaction for astrophysical purposes L. Csedreki1, G. F. Ciani2, I. Kochanek1 for the LUNA collaboration 1 INFN, Laboratori Nazionali del Gran Sasso LNGS, Assergi, Italy 2 Gran Sasso Science Institute, L’Aquila Contact email: csedreki.laszlo@lngs.infn.it The 13C(α,n)16O reaction is very important in astrophysical context. This reaction is the dominant neutron source for the synthesis of the main s-process component of heavy elements in thermally pulsing, low-mass asymptotic giant branch stars. As a new project at the LUNA 400 kV accelerator, the investigation of this reaction is being performed in the Laboratori Nazionali del Gran Sasso (LNGS), Italy. This underground laboratory provides an ideal environment to detect rare events from astrophysical reactions thanks to the strong reduction in cosmic-ray induced background. For the above mentioned purpose the experimental setup needs to be able to detect the reaction neutrons with high efficiency, also considering possible angular distributions. Multistage target holder, high capacity cooling system and the implementation of the in-beam checking of target thickness is also required. Moreover, due to the low cross section of the 13C(α,n)16O reaction in the planned alpha energy range, the minimization of environmental and beam induced background are essential. The poster introduces the design and the parameters of the experimental setup including the process of target composition analysis using various techniques.
Speaker: Mr Laszlo Csedreki (INFN LNGS)
• 19:30
Measurements of the 10B(p,α0) 7Be cross section at astrophysical energies using the Trojan Horse Method 2h
For nucleosynthesis calculations precise reaction rates should be known at energies close to the Gamow peak. Accurate measurements of nuclear reactions performed at these energies [1-5] shows an unexpected enhancement of the cross section at the lowest measurable energies that is attributed to the presence of atomic electrons in the target. In order to observe the bare nuclear cross section, it is possible to perform experiments where the cross section is measured indirectly, as for example with the Trojan Horse Method (THM). In this method the electron screening effect is neglected since the measurements take place at much higher energies [6]. The THM has been applied to the quasifree 2H(10B,α_0,7Be)n reaction induced at a boron-beam energy of 28 MeV. The astrophysical S-factor of the 10B(p,α_0)7Be reaction was measured in a wide energy range, from 5 keV to 2.5 MeV. In this experiment has been achieved a much better energy resolution as compared to the previous one [7] allowing the significantly better separation of the 8.654 MeV and 8.699 MeV 11C levels. Since the 8.699 MeV resonance lies at the Gamow peak energy for the 10B(p,α)7Be reaction, the proper subtraction of events belonging to the subthreshold level at the 8.654 MeV is necessary for accurate determination of the astrophysical S-factor and so, electron screening potential. [1] C. Rolfs, W.Rodney, Cauldrons in the Cosmos, The University of Chicago, 561 (1988); [2] H. Assenbaum et al., Z. Phys. A 327, 461 (1987); [3] G. Fiorentini et al., Z. Phys. A 350, 289 (1995); [4] F. Strieder et al., Naturwissenschaften 88, 461 (2001); [5]E. G. Adelberger et al., Rev. Mod. Phys. 195, 83 (2011); [6] S. Typel, H. H. Wolter, Few-Body Systems 29, 75 (2000); [7] C.Spitaleri et al., Phys. Rev. C 90, 035801 (2014).
Speaker: Mrs Aleksandra Cvetinović (INFN-LNS Catania)
• 19:30
Nanostructured surfaces for nuclear astrophysics studies by laser-matter interactions 2h
The future availability of high-intensity laser facilities capable of delivering tens of Petawatts of power (e.g. ELI-NP) into small volumes of matter at high repetition rates will give the unique opportunity to investigate nuclear reactions and fundamental interactions under the extreme plasma conditions realized by laser-matter interactions. Nuclear reactions of astrophysical interest are typically investigated by using ion beams that collide on fixed targets. However, the universe is composed of matter mainly in the form of plasma, where reaction mechanisms could change dramatically. For this reason, the investigation on reaction rates in plasma could provide important knowledge in astrophysics and cosmology. In this context, targets made of nanostructured materials are giving promising indications to reproduce plasma conditions suitable for measurements of thermonuclear fusion reaction rates, in the domain of nanosecond laser pulses. The present work gives the results of measurements performed with several kinds of nanostructured targets irradiated by laser pulses 6 ns long and at the energy of 2 Joules. The Nd:YAG laser installed at LENS laboratory of INFN-LNS in Catania has been used. The nanostructured targets consist of aligned metal nanowires grown by electrodeposition into a porous alumina matrix, obtained on a thick aluminum substrate. These metamaterials were developed with specific geometrical parameters in order to maximize absorption in the visible and IR range. A strong enhancement of the plasma-produced X-ray flux has been observed, with some clear signatures about a “stagnation” of the plasma plume which is a critical condition for the self-thermalization of the system. In perspective, this kind of alumina matrices could be filled with the atomic species needed to investigate specific nuclear reactions, in laser-produced plasmas.
Speaker: Carmen Altana (LNS)
• 19:30
Neutron capture cross sections of Kr 2h
% % Nuclear Physics in Astrophysics 8 template for abstract % % Format: LaTeX2e. % % Rename this file to name.tex, where name' is the family name % of the first author, and edit it to produce your abstract. % \documentstyle[11pt]{article} % % PAGE LAYOUT: % \textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset -0.35in \topmargin 0.305in \oddsidemargin +0.35in \evensidemargin -0.35in %\renewcommand{\rmdefault}{ptm} % to use Times font \long\def\TITLE#1{{\Large{\bf#1}}}\long\def\AUTHORS#1{ #1\\[3mm]} \long\def\AFFILIATION#1#2{$^{#1}\,$ #2\\} \begin{document} {\small \it Nuclear Physics in Astrophysics 8, NPA8: 18-23 June 2017, Catania, Italy} \vspace{12pt} \thispagestyle{empty} \begin{center} %%% %%% Title goes here. %%% \TITLE{Neutron capture cross sections of Kr}\\[3mm] %%% %%% Authors and affiliations are next. The presenter should be %%% underlined as shown below. %%% \AUTHORS{S. Fiebiger$^{1}$, B. Baramsai$^{2}$, A. Couture$^{2}$, S. Mosby$^{2}$, J. M. O'Donnell$^{2}$, R. Reifarth$^{1}$, G. Rusev$^{2}$, J. Ullmann$^{2}$, M. Weigand$^{1}$, C. Wolf$^{1}$} %%% {\small \it \AFFILIATION{1}{Goethe University Frankfurt, Germany} \AFFILIATION{2}{Los Alamos National Laboratory, USA} } %%% \vspace{12pt} % Do not modify % Enter contact e-mail address here. \centerline{Contact email: {\it fiebiger@iap.uni-frankfurt.de}} \vspace{18pt} % Do not modify \end{center} %%% %%% Abstract proper starts here. %%% Neutron capture and $\beta^{-}$-decay are competing branches of the s-process nucleosynthesis path at $^{85}$Kr [1], which makes it an important branching point. The knowledge of its neutron capture cross section is therefore essential to constrain stellar models of nucleosynthesis. Despite its importance for different fields, no direct measurement of the cross section of $^{85}$Kr in the keV-regime has been performed. The currently reported uncertainties are still in the order of 50\% [2, 3]. Neutron capture cross section measurements on a 4\% enriched $^{85}$Kr gas enclosed in a stainless steel cylinder were performed at Los Alamos National Laboratory (LANL). Using the Detector for Advanced Neutron Capture Experiments (DANCE), a 162 times segmented BaF$_2$ scintillator array. This segmentation combined with a high efficiency allows measurements on small samples of radioactive isotopes. $^{85}$Kr is radioactive isotope with a half life of 10.8 years. As this was a low-enrichment sample, the main contaminants, the stable krypton isotpes, $^{83}$Kr and $^{86}$Kr were also investigated. The material was highly enchriched and contained in pressurized stainless steel spheres. \bigskip {\small \noindent [1] C. Abia et al. Astrophysical Journal, 559:1117 (2001); \noindent [2] R. Raut et al. Cross-Section Measurements of the 86Kr(g,n) Reaction to Probe the s-Process Branching at 85Kr (2013); \noindent [3] Z. Y. Bao et al. Atomic Data Nucl. Data Tables, 76:70 (2000) %\noindent [1] E. Stark, Phys. Journal of the North 83 045801 (2011); %\noindent %[2] O. Martell et al. submitted to Solar Physics Letters (2013).} %%% %%% End of abstract. %%% \end{document}
Speaker: Mr Stefan Fiebiger (Goethe University Frankfurt)
• 19:30
Search for Deeply Bound Kaonic Nuclear States in AMADEUS experiment 2h
Search for Deeply Bound Kaonic Nuclear States in AMADEUS experiment M. Skurzok1,2, C. Curceanu2, L. Fabbietti3,4, R. del Grande2,5, P. Moskal1, K. Piscicchia2,6, A. Scordo2, D. L. Sirghi2, Oton Vazquez Doce3,4 1 Institute of Physics, Jagiellonian University, 30-059 Krakow, Poland 2 INFN, Laboratori Nazionali di Frascati, 00044 Frascati, Italy 3 Excellence Cluster Origin and Structure of the Universe, 85748 Garching, Germany 4 Physik Department E12, Technische Universitat Munchen, 85748 Garching, Germany 5 Università degli Studi di Roma Tor Vergata, Rome, Italy 6 Museo Storico della Fisica e Centro Studi e Ricerche Enrico Fermi, Roma, Italy Contact email: magdalena.skurzok@uj.edu.pl Deeply Bound Kaonic Nuclear States are currently one of the hottest topics in nuclear and hadronic strangeness physics, both from experimental and theoretical points of view. The existence of bound kaonic nuclear states of K−, also called kaonic nuclear clusters, was firstly predicted in 1986 [1]. The phenomenological investigations, resulted in deeply bound nuclear states with narrow widths and large binding energies which can reach 100 MeV in kaon-nucleon-nucleon system (K−pp), being a consequence of the strongly attractive K− - proton interaction. Recent theoretical studies, based on different methods are giving a wide range of possible values for the binding energies of the kaonic nuclear states, ranging from few MeV up to about 100 MeV [2-5]. Therefore, in order to clarify this issue, experimental data are needed. The research would be very important in understanding the fundamental laws of the Nature and Universe. It can have important consequences in various sectors of physics, like nuclear and particle physics as well as astrophysics. The binding of the kaon in nuclear medium may impact on models describing the structure of neutron stars (Equation of State of neutron stars) [6,7] including binaries which are expected to be sources of the gravitational waves. Investigation of stable forms of strange matter like DBKNS in extreme conditions would be helpful for a better understanding of elementary kaon - nucleon interaction for low energies in the non-perturbative quantum chromodynamics (QCD) and in consequence, would contribute to solve one of the crucial problems in hadron physics: hadron masses (related to the chiral symmetry breaking), hadron interactions in nuclear medium and the structure of the dense nuclear matter. The AMADEUS group has developed a method having a high chance for discovery of DBKNS corresponding to K−pp, K−ppn and K−ppnn kaonic nuclear clusters and their decay to Λp, Λd and Λt, respectively. The method is based on the exclusive measurement of the momentum, angular and invariant mass spectra for correlated Λp, Λd, Λt [8]. Possible DBKNS may be produced with K− stopped in helium or carbon and then decay into considered decay channels. The experiment was carried out with very high precision and high acceptance by AMADEUS using the KLOE detector itself as an active target (2004-2005) as well as with dedicated high purity graphite target (2012) and using low-energetic negatively charged kaon beam provided by DAΦNE collider located in National Laboratory in Frascati (Italy). The poster will present status of the data analysis. [1] S. Wycech, Nucl. Phys. A 450 399c (1986); [2] Y. Akaishi, T. Yamazaki, Phys. Lett. B 535 70 (2002); [3] A. Dote, T. Hyodo, W. Weise, Phys. Rev. C 79 014003 (2009); [4] N. V. Shevchenko, A. Gal, J. Mares, Phys. Rev. Lett. 98 082301 (2007); [5] Y. Ikeda, T. Sato, Phys. Rev. C 79 035201 (2009); [6] A. E. Nelson and D. B. Kaplan, Phys. Lett B 192 193 (1987); [7] A. Scordo, et al., AIP Conf. Proc. 1735 080015 (2016); [8] C. Curceanu, et al., Acta Phys. Polon. B 46 203 (2015).
Speaker: Ms Magdalena Skurzok (Jagiellonian University)
• 19:30
Study of alpha cluster states in light nuclei for nuclear physics and astrophysics 2h
% Nuclear Physics in Astrophysics 8 template for abstract % % Format: LaTeX2e. % % Rename this file to name.tex, where name' is the family name % of the first author, and edit it to produce your abstract. % \documentstyle[11pt]{article} % % PAGE LAYOUT: % \textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset -0.35in \topmargin 0.305in \oddsidemargin +0.35in \evensidemargin -0.35in %\renewcommand{\rmdefault}{ptm} % to use Times font \long\def\TITLE#1{{\Large{\bf#1}}}\long\def\AUTHORS#1{ #1\\[3mm]} \long\def\AFFILIATION#1#2{$^{#1}\,$ #2\\} \begin{document} {\small \it Nuclear Physics in Astrophysics 8, NPA8: 18-23 June 2017, Catania, Italy} \vspace{12pt} \thispagestyle{empty} \begin{center} %%% %%% Title goes here. %%% \TITLE{Study of alpha cluster states in light nuclei for nuclear physics and astrophysics.}\\[3mm] %%% %%% Authors and affiliations are next. The presenter should be %%% underlined as shown below. %%% \AUTHORS{A.K.Nurmukhanbetova$^1$, V.Z. Goldberg$^2$, D.K. Nauruzbayev$^{1,5}$, M.S.Golovkov$^3$, A.Volya$^4$,G.V.Rogachev$^2$ } %%% {\small \it \AFFILIATION{1}{National Laboratory Astana, Nazarbayev University, Astana, 010000,Kazakhstan} \AFFILIATION{2}{Cyclotron Institute, Texas A$\&$M University, College Station, Texas, USA} \AFFILIATION{3}{Joint Institute of Nuclear Research, Dubna, Russian} \AFFILIATION{4}{Department of Physics, Florida State University, Tallahassee, Florida 32306, USA} \AFFILIATION{5}{Saint Petersburg State University, Saint Petersburg, Russia} } %%% \vspace{12pt} % Do not modify % Enter contact e-mail address here. \centerline{Contact email: {\it anurmukhanbetova@nu.edu.kz}} \vspace{18pt} % Do not modify \end{center} %%% %%% Abstract proper starts here. %%% It is well recognized that current interest in $\alpha$ particle interaction with nuclei is strongly motivated by astrophysics [1]. Even if astrophysical reactions involving helium do not proceed through the strong $\alpha$-cluster states (because of their high excitation energy), these states can provide α width to the levels that are closer to the region of astrophysical interest through configuration mixing. We used a low energy heavy ion cyclotron in Astana (Kazakhstan) to study resonance reactions induced by ions of \textsuperscript{13}C[2], \textsuperscript{15}N[3],\textsuperscript{16}O, \textsuperscript{17}O in helium and hydrogen gas target. The Thick Target Inverse Kinematics Method [3,4,5] was used to obtain the continuous in energy excitation functions in the large angular interval using 1.9 MeV/u initial energy of the accelerated ions. The experimental excitation functions were analyzed using multilevel multichannel R matrix code [6], and the data on over 100 levels were obtained. We did not use any background resonances in the fit. New data were obtained even for a well-studied case \textsuperscript{20}Ne nucleus populated in the \textsuperscript{16}O+ $\alpha$ resonance elastic scattering. The \textsuperscript{17}O+ $\alpha$ resonance elastic scattering has not been studied before. The nuclear structure theoretical calculations were made in the framework of the cluster-nucleon configuration interaction model [7]. In the talk we present the experimental results (Fig.1.), evaluate a shell model approach progress in the description of the cluster states, and consider modifications and a possible progress of the experimental approach. \begin{figure}[h] \centering \includegraphics{fig-1-NPA8.jpeg} \caption{The 180$^\circ$ excitation function for the \textsuperscript{16}O+ $\alpha$ resonance elastic scattering together with R matrix fit.} \label{fig:awesome_image2} \end{figure} \bigskip {\small \noindent [1] A. Aprahamian et al. Nuclear structure aspects in nuclear astrophysics, Progress in Particle and Nuclear Physics. 54 (2005) 535–613. doi:10.1016/j.ppnp.2004.09.002; \noindent [2] N.A.Mynbayev et al. J.Exper.Theo.Phys. 119, 663 (2014); Zh.Eksp.Teor.Fiz. 146, 754 (2014); \noindent [3] A.K. Nurmukhanbetova et al. Implementation of TTIK method and time of flight for resonance reaction studies at heavy ion accelerator DC-60, Nuclear Instruments and Methods in Physics Research Section A: Accelerators, Spectrometers, Detectors and Associated Equipment. 847 (2017) 125–129. doi:10.1016/j.nima.2016.11.053; \noindent [4] K. P. Artemov, et al., Sov. J. Nucl. Phys. 52, 634 (1990); \noindent [5] G. V. Rogachev, et. al AIP Conf. Proc. 1213, 137 (2010); \noindent [6] E.D.Johnson, Ph.D. thesis, Florida State University, 2013; \noindent [7] A. Volya et al. Nuclear clustering using a modern shell model approach, Physical Review C. 91 (2015) 44319. doi:10.1103/PhysRevC.91.044319. } %%% %%% End of abstract. %%% \end{document}
Speakers: Dr Aliya Nurmukhanbetova (National Laboratory Astana, Nazarbayev University, Astana, 010000,Kazakhstan), Mr Dosbol Nauruzbayev (National Laboratory Astana, Nazarbayev University, Astana, 010000,Kazakhstan)
• 19:30
Sub-barrier fusion cross section measurements with STELLA 2h
The STELLA (STELlar LAboratory) experimental station for the measurement of sub-barrier light heavy ion fusion cross sections has been commissioned at the Androm\{e}de accelerator at IPN, Orsay. These measurements can yield both insight into nuclear cluster effects~[1] and the $S$-factors at energies of astrophysical interest. In particular, $^{12}$C+$^{12}$C fusion was identified as a key reaction on the production route of heavier elements in massive stars during the carbon burning phase, in type Ia supernovae and in superbursts from accreting neutron stars~[2]. Since sub-barrier fusion reactions are strongly hindered by Coulomb repulsion, the experimental determination of these cross sections ($\sim$~nb) is highly challenging. Nowadays, the determination of such cross sections is targeted with coincidence measurements using the so called gamma-particle-technique~[3]. The STELLA setup comprises a set of DSSSDs as well as an array of LaBr$_{3}$ detectors from the UK FATIMA collaboration (FAst TIMing Array) for charged particle and gamma recognition, respectively. In addition, a rotating target mechanism is developed to sustain beam intensities $>10\mu$A. In this contribution, the experimental layout will be introduced in detail with a focus on the design and performance of LaBr$_{3}$ detection array. Furthermore, the measurement technique will be sketched with first results from the commissioning campaign using $^{12}$C beam. [1] D.~Jenkins and S.~Courtin, Phys. Jour. G 42, 034010 (2015); [2] L.R.~Gasques \textit{et al.}, PRC 76, 3, 035802 (2007); [3] C.L.~Jiang \textit{et al.}, NIM A 682, 12 (2012);
Speaker: Prof. Sandrine Courtin (IPHC Strasbourg)
• 19:30
The Measurement of Long Lived Alpha Decay for Cosmochronometry 2h
% % Nuclear Physics in Astrophysics 8 template for abstract % % Format: LaTeX2e. % % Rename this file to name.tex, where name' is the family name % of the first author, and edit it to produce your abstract. % \documentstyle[11pt]{article} % % PAGE LAYOUT: % \textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset -0.35in \topmargin 0.305in \oddsidemargin +0.35in \evensidemargin -0.35in %\renewcommand{\rmdefault}{ptm} % to use Times font \long\def\TITLE#1{{\Large{\bf#1}}}\long\def\AUTHORS#1{ #1\\[3mm]} \long\def\AFFILIATION#1#2{$^{#1}\,$ #2\\} \begin{document} {\small \it Nuclear Physics in Astrophysics 8, NPA8: 18-23 June 2017, Catania, Italy} \vspace{12pt} \thispagestyle{empty} \begin{center} %%% %%% Title goes here. %%% \TITLE{The Measurement of Long Lived Alpha Decay for Cosmochronometry}\\[3mm] %%% %%% Authors and affiliations are next. The presenter should be %%% underlined as shown below. %%% \AUTHORS{Heinrich Wilsenach$^1$, Kai Zuber$^1$, R\'ene Heller$^2$, Volker Neu$^3$, Yordan Georgiev$^4$, and Tommy Sch\"onherr$^4$} %%% {\small \it \AFFILIATION{1}{IKTP TU-Dresden, Dresden, Germany} \AFFILIATION{2}{Institute of Ion Beam Physics and Materials Research, Dresden-Rossendorf, Germany} \AFFILIATION{3}{Institute for Metallic Materials, Dresden, Germany} \AFFILIATION{4}{Transport Phenomena in Nanostructures, Dresden-Rossendorf, Germany} } %%% \vspace{12pt} % Do not modify % Enter contact e-mail address here. \centerline{Contact email: {\it heinrich.wilsenach@tu-dresden.de}} \vspace{18pt} % Do not modify \end{center} %%% %%% Abstract proper starts here. %%% Alpha decay has historically given insight into the inner workings of the nucleus as the decay rate is strongly affected by nuclear structure. Very long lived alpha decaying isotopes (about T$_{1/2}$ = 10$^{8-10}$ a) can be used as a powerful tool to date the formation of astronomical objects in the Solar System due to their extremely long half lives. This technique is however very vulnerable to the accuracy of the half-life. This means that improved half-live measurements are important though they pose a significant technical obstacle. To measure the half-lives of such long lived isotopes besides appropriate targets special care needs to be taken with background and signal efficiency. To overcome these obstacles the design of the twin Frisch-Grid ionisation chamber was chosen [1]. This design combines excellent energy resolution with a hight detector efficiency and the usage of radio-pure materials to measure decay rates in the region of a few counts per day. It is also possible to use pulse shape analysis to obtain position information on each event, allowing for improved signal to background discrimination. This presentation will give an overview of the detection aspects of the twin Frisch-Grid ionisation chamber, as well as the calibrations that were performed. New measurements of the half-lives of $^{147}$Sm and $^{190}$Pt will also be presented and discussed here. \bigskip {\small \noindent [1] A. Hartmann et al., NIM A 814, 12 (2016). %\noindent[2] O. Martell et al. submitted to Solar Physics Letters (2013).} %%% %%% End of abstract. %%% \end{document}
Speaker: Mr Heinrich Wilsenach (TU-Dresden, IKTP)
• 19:30
The role of $^{13}$C excited states in $\alpha+^{9}$Be reaction and scattering cross sections 2h
The study of $^{13}$C structure allows to understand the effects of clusterization in light non-self-conjugated nuclei. The possible presence of rotational bands built on molecular states has been suggested in several papers [1,2]. Furthermore, in recent times, some theoretical papers [3,4] predicted the possible existence of states corresponding to the coupling of a valence neutrons to the $^{12}$C Hoyle state. To shed light on these aspects, we performed a comprehensive $R$-matrix fit of $\alpha+^{9}$Be elastic ($\alpha_0$) and inelastic ($\alpha_1$ and $\alpha_2$) scattering data in the energy range E$\simeq$ 3.5 – 10 MeV at several angles [5]. To carefully determine the partial decay widths of states above the $\alpha$ decay threshold we included in the fit procedure also $^{9}$Be($\alpha,n_0$)$^{12}$C$_{gs}$ and $^{9}$Be($\alpha,n_1$)$^{12}$C$_{4.44}$ cross section data taken from [6,7]. This analysis allows to improve the (poorly known) spectroscopy of excited states in $^{13}$C in the E$_x\simeq$12-17 MeV region [8]. Furthermore, a better knowledge of high-energy resonance parameters (especially for broad states) can improve low-energy extrapolations of the $^{9}$Be($\alpha,n$)$^{12}$C reaction $S$-factor, that plays a key role in the description of $^{12}$C nucleosynthesis during a supernova explosions [7,9]. Preliminary results of these studies will be discussed. \bigskip {\small \noindent [1] M. Milin and W. von Oertzen, Eur. Phys. J. A 14 (2202) 295.\\ \noindent [2] N. Furutachi and M. Kimura, Phys. Rev. C 83 (2011) 021303(R).\\ \noindent [3] T. Yamada and Y. Funaki, Phys. Rev. C 92 (2015) 034326.\\ \noindent [4] Y. Chiba and M. Kimura, J. Phys.: Conf. Ser. 569 (2014) 012047.\\ \noindent [5] I. Lombardo et al., Nucl. Instr. Meth. Phys. Res. B 302 (2013) 19.\\ \noindent [6] L. van der Zwan and K. W. Geiger, Nucl. Phys. A 152 (1970) 481.\\ \noindent [7] R. Kunz et al., Phys. Rev. C 53 (1996) 2486.\\ \noindent [8] M. Freer et al., Phys. Rev. C 84 (2011) 034317.\\ \noindent [9] S.E. Woosley and R.D. Hoffman, Astrophys. J. 395 (1992) 202.\\
Speaker: Dr Ivano Lombardo (Università di Napoli Federico II and INFN - Sez. Napoli)
• 19:30
Treatment of isomers in nucleosynthesis codes 2h
Isomers are metastable states of atomic nuclei. Their half-lifes are about 100 to 1000 times longer than those of the excited nuclear states with prompt g-emissions. If the conditions in an application change on the time scale of isomers' half lifes, their abundances have to be tracked explicitly. The high temperatures under stellar conditions enable the population of higher-lying states via thermal excitations. These states either decay back or populate different states, e.g isomers. Isomers are particular important if their $\beta$-decay rates differ amongst each other. As a result, the effective life-time of an isotope under stellar conditions can differ dramatically from terrestrial conditions. In stellar nucleosynthesis codes, environmental conditions change on time scales ranging from milliseconds during explosions to millions of years during the burning phases. Hence, the treatment of isomers depends on the investigated scenario. We will present a general approach to the treatment of isomers in hot, thermalized environments with a special emphasis on the impact on stellar nucleosynthesis. Important examples like $^{26}$Al and $^{85}$Kr will be discussed.
Speaker: Prof. Rene Reifarth (Goethe University Frankfurt)
• 19:30
“Development and use of CR39 Nuclear Track Detectors for the Measurement of the Interaction of (High Flux) Neutron Beams with 7Be and the Primordial 7Li problem 2h
% % Nuclear Physics in Astrophysics 8 template for abstract % % Format: LaTeX2e. % % Rename this file to name.tex, where name' is the family name % of the first author, and edit it to produce your abstract. % \documentstyle[11pt]{article} % % PAGE LAYOUT: % \textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset -0.35in \topmargin 0.305in \oddsidemargin +0.35in \evensidemargin -0.35in %\renewcommand{\rmdefault}{ptm} % to use Times font \long\def\TITLE#1{{\Large{\bf#1}}}\long\def\AUTHORS#1{ #1\\[3mm]} \long\def\AFFILIATION#1#2{$^{#1}\,$ #2\\} \begin{document} {\small \it Nuclear Physics in Astrophysics 8, NPA8: 18-23 June 2017, Catania, Italy} \vspace{12pt} \thispagestyle{empty} \begin{center} %%% %%% Title goes here. %%% \TITLE{Development and use of CR39 Nuclear Track Detectors for the Measurement of the Interaction of (High Flux) Neutron Beams with $^7$Be and the Primordial $^7$Li problem$^*$" }\\[3mm] %%% %%% Authors and affiliations are next. The presenter should be %%% underlined as shown below. %%% \AUTHORS{E. E. Kading$^1$, M. Tessler$^2$, E.A. Maugeri$^3$, O. Aviv$^4$, M. Ayranov$^3$, D. Berkovits$^4$, R. Dressler$^3$, I. Eliyahu$^4$, M. Gai$^1$, S. Halfon$^4$, M. Hass$^5$, S. Heinitz$^3$, C.R. Howell$^6$, D. Kijel$^4$, N. Kivel$^3$, U. Koester$^7$, I. Mardor$^4$, Y. Mishnayot$^4$, I. Mukul$^5$, T. Palchan$^2$, A. Perry$^4$, Y. Shachar$^5$, D. Schumann$^3$, Ch. Steiffert$^8$, A. Shor$^4$, I. Silverman$^4$, S.R. Stern$^1$, Th. Stora$^8$, D.R. Ticehurst$^6$, A. Weiss$^{9,10}$, L. Weissman$^4$} %%% {\small \it \AFFILIATION{1}{LNS at Avery Point, University of Connecticut, Groton, CT 06340, USA.} \AFFILIATION{2}{Racah Institute of Physics, The Hebrew University, Jerusalem, 91904.} \AFFILIATION{3}{Laboratory for Radiochemistry, Paul Scherrer Institute, CH-5232 Villigen, Switzerland.} \AFFILIATION{4}{Soreq Nuclear Research Center, Nuclear Physics Engineering Division, Yavne 81800, Israel.} \AFFILIATION{6}{TUNL, Department of Physics, Duke University, Durham, North Carolina 27708-0308.} \AFFILIATION{7}{Institut Laue-Langevin, 38000 Grenoble, France.} \AFFILIATION{8}{ISOLDE, CERN, CH-1211 Geneva, Switzerland.} \AFFILIATION{9}{Faculty of Engineering, Bar Ilan University, Ramat Gan 52900, Israel.} \AFFILIATION{10}{Bio-Imaging Unit, Institute for Life Sciences, Hebrew University, Jerusalem, 91904, Israel.}} %%% \vspace{12pt} % Do not modify % Enter contact e-mail address here. \centerline{Contact email: {\it emily.kading@uconn.edu}} \vspace{18pt} % Do not modify \end{center} %%% %%% Abstract proper starts here. %%% The high intensity epithermal neutron beams produced by the Soreq Applied Research Accelerator Facility (SARAF) operating with the Liquid Lithium Target (LiLiT) present significant opportunities in Nuclear Astrophysics. However, major experimental challenges arise when a detector is used with the high flux 50 keV quasi-Maxwellian neutron beams produced by the LiLiT ($\sim 10^{10}$ n/sec/cm$^2$) as well as the high flux ($\sim 10^{11}$ /sec) of 477 keV gamma-rays from the $^7$Li(p,p'$\gamma$) reaction. We are developing protocols [1] for the use of CR39 Nuclear Track Detectors (NTD) in such high intensity backgrounds. We calibrated CR39 NTD with alpha-particles from standard radioactive sources and by using Rutherford Backscattering of accelerated alpha-particles and protons from a thin gold foil. We used cold neutrons to calibrate the background" $^{17}$O(n,$\alpha$) reaction that occurs inside the CR39 plates. The plates were etched in a standard 6.25 N NaOH solution for 30 minutes at 90$^{\circ}$C to produce micron size circular pits. The plates were scanned with a fully motorized microscope. A segmentation algorithm that addresses the challenges posed by the intense neutron beam and gamma-ray background was developed. We used a (phantom") $^9$Be target produced at the Paul Scherrer Institute(PSI) [2] to measure the background from irradiation with an intense ($\sim 10^{10}$ n/cm$^2$/sec) neutron beam. Using our calibration we define the radii region of interest (RRI) for detecting alpha-particles and we demonstrate that it is governed by pits generated by the combination of 1.4 - 1.7 MeV alpha-particles and 0.6 - 0.3 MeV $^{14}$C from the $^{17}$O(n,$\alpha$)$^{14}$C reaction that occurs inside the CR39. These backgrounds are the limiting factor in measuring small cross sections with the current setup, as for example is required in the study of the interaction of neutrons with $^7$Be, which is important for understanding the Primordial $^7$Li Problem" [3]. \\ \ \\ $^*$ Work supported by the U.S.-Israel Bi National Science Foundation, Award Number 2012098, and the U.S. Department of Energy, Award Number DE-FG02-94ER40870. \bigskip {\small \noindent [1] Emily Elizabeth Kading {\em et al.}, to be published, Jour. Instr. (2017). \noindent [2] Emilio Andrea Maugeri {\em et al.}, in press, Jour. Instr. (2017) \noindent [3] Moshe Gai, Invited Talk, this conference. %%% %%% End of abstract. %%% \end{document}
• Wednesday, 21 June
• 08:30 11:00
Nuclear astrophysics with lasers Sala conferenze

### Sala conferenze

#### Laboratori Nazionali del Sud

Via S. Sofia 62 I-95123 Catania Italy
• 08:30
Nuclear physics and astrophysics ELI-NP: The emerging future 30m
The mission of the Extreme Light Infrastructure Nuclear Physics (ELI-NP) research infrastruc- ture are nuclear physics studies with high-power lasers and high-brilliance quasi-monochromatic gamma beams [1,2]. The laboratory will become operational as an user facility in 2019. Two high-power lasers will provide laser pulses on target, each of them having three outputs, e.g. of100TWat10Hz,1PWat1Hzand10PWonceperminute. Thetwolaserarmswillbe synchronized and it will be possible to deliver any combination of these pulses on target, since each output will be provided with its own amplifier [3]. In addition, a high-brilliance narrow- bandwidth gamma beam will be produced at ELI-NP via Compton backscattering of laser light off electrons accelerated to relativistic energies [4]. The 100 Hz electron bunches will be delivered by an electron linac, where they will be accelerated up to energies of 750 MeV. There will be two interaction points where the electrons will collide with laser pulses provided by 0.2 J 100 Hz Yb:YAG lasers. At one of them, a low-energy gamma beam will be produced, with energies up tp 3.5 MeV, and at the other one the maximal energy of the gamma beam will reach 19.5 MeV. Each electron bunch will consist of a train of 32 microbunches and laser re-circulators will be used at the interaction points to ensure the interaction of the laser pulse with each of the bunches in the train. Thus, gamma beams of spectral density of 104 photons/s/eV will be produced, which after collimation results in highly polarized (¿ 95%)quasi-monochromatic gamma beams (bandwidth le0.5%) with beam intensities of 1010 photons/s, or ∼ 109 per microbunch. Several types of experiments will be possible at ELI-NP, e.g. laser-driven experiments in single or double pulse-shot mode on target, gamma-beam experiments in narrow- or wide- bandwidth mode, and combined laser- and gamma-beam experiments. Thus, the ELI-NP labo- ratory opens a new dimension for nuclear physics studies with intense electromagnetic probes. The experimental program, which is under preparation at ELI-NP targets all these experimental modes and at present a large variety of instruments are under construction [2,5,6]. The present status of the implementation facility, as well as the emerging experimental program in the field of nuclear physics and astrophysics will be described, with an emphasis of the considered day-one experiments. [1] N. V. Zamfir, Nucl. Phys. News 25:3 34 (2015); [2] S. Gales et al., Phys. Scr. 91 093004 (2016); [3] N. V. Zamfir, Eur. Phys. J. Special Topics 223 1221 (2014) [4] O. Adriani et al., arXiv:1407.3669 [physics.acc-ph] (2014); [5] ELI-NP TDR teams, Rom. Rep. Phys. 68S (2016) (www.rrp.infim.ro); [6] D. L. Balabsnki et al., Europhys. Lett. 117 28001 (2017).
Speaker: Prof. Dimiter Balabanski (ELI-NP/IFIN)
• 09:00
Investigating nuclear reactions at astrophysical energies with gamma-ray beams and an active-target TPC 30m
A new methodology to measure cross-sections for thermonuclear reactions that power the stars is being developed at the University of Warsaw. These reactions take place at different energies according to the respective stellar environment. Such energies are well below the Coulomb barrier and the respective cross-sections are incredibly small, often below the experimental reach. There is a lack of experimental data on cross-sections for low-energies, information that is indispensable for modelling energy production in stars. As a consequence, extrapolations are made, with their unavoidable large uncertainty. Of special interest are (p,gamma) and (alpha,gamma) reactions, in particular those, that regulate the ratio of C and O and those that burn 18O and, therefore, regulate the ratio between 16O and 18O in the Universe. One of the benchmark reactions to be investigated in this work is the 12C(alpha,gamma)16O at energies down to 1 MeV in the centre-of-mass reference frame. We propose to use a gaseous active target detector to study (alpha,gamma) and (p,gamma) nuclear reactions of current astrophysical interest by means of studying time-inverse photo-disintegration processes induced by high energy photons. The advantage of such an approach stems from the fact that photons are not subject to the nuclear Coulomb barrier. The Extreme Light Infrastructure-Nuclear Physics facility (ELI-NP) - currently being built near Bucharest, Romania - will deliver monochromatic, high-brilliance and polarized gamma-ray beams. The charged products of photodisintegration reactions will be measured by means of a Time Projection Chamber (ELITPC) with 3-coordinate (u-v-w) planar electronic readout acting as virtual pixels. The detector will be equipped with triple-GEM structure for gas amplification and will work at lower-than-atmospheric pressure. The concept of the detector and the status of the R&D for it will be presented, as well as results from tests using a scaled demonstrator detector.
Speaker: Dr Chiara Mazzocchi (University of Warsaw)
• 09:30
Fusion plasmas and neutron production from the interaction of D2 and CD4 clusters with contrast upgraded Texas Petawatt laser 30m
Nuclear fusion from the interaction of very high intensity laser pulses and nm-scale deuterium clusters has been studied since 1999 [1]. These van der Waals bonded clusters can be easily produced in the expansion of a gas jet into vacuum. They absorb the laser pulse energy very efficiently (approaching 100% under certain conditions) and the process by which the ions attain high kinetic energies has been well explained by the Coulomb explosion model. Using these energetic exploding clusters, it is possible to create fusion plasmas with ion temperatures of many keV at densities of up to 1019 cm−3. DD fusion events occur between ions or when energetic ions collide with cold atoms in the background gas jet. As a result of both of these fusion reactions, quasi-monoenergetic 2.45 MeV neutrons are produced from the localized fusion plasma in a sub-nanosecond burst becoming an attractive bright, short, and localized neutron source potentially useful for material damage. These plasmas have been exploited to measure the astrophysical S factor for the 3He(d,p)4He fusion reaction at temperatures of few keV by irradiating a D2-3He mixture [2]. In this talk, I will review several experiments performed using the Texas Petawatt laser to measure astrophysical S-factors [3] and to optimize the neutron yield using D2 and CD4 clusters where 2·107n/shot were achieved [4]. Previous experiments showed a drop in the ion temperature with high laser intensities suggesting laser pre-pulses could be breaking the clusters before arrival of the main pulse [5]. In 2015, the Texas Petawatt laser underwent a major upgrade to its pulse contrast to reduce the intensity of pre-pulses [6]. I will present our recent results in neutron yield with the contrast upgraded Texas Petawatt laser and discuss measurements of the ion range in cluster media that we found differs considerably from that of homogeneous gases [7]. [1] T. Ditmire et al., Nature (London) 398, 489 (1999). [2] M. Barbui et al., Phys. Rev. Lett. 111, 082502 (2013). [3] D. Lattuada et al., Phys. Rev. C 93, 045808 (2016). [4] W. Bang et al., Phys. Rev. E 87, 023106 (2013). [5] W. Bang et al., Phys. Rev. E 87, 023106 (2013). [6] E. Gaul et al., J. Phys. Conf. Ser. 717, 012092 (2016). [7] G. Zhang et al., Phys. Lett. A 381, 1682 (2017).
Speaker: Dr Hernan J. Quevedo (University of Texas)
• 10:00
Measurements Of Stellar And Big-Bang Nucleosynthesis Reactions Using Inertially-Confined Plasmas 20m
% % Nuclear Physics in Astrophysics 8 template for abstract % % Format: LaTeX2e. % % Rename this file to name.tex, where name' is the family name % of the first author, and edit it to produce your abstract. % \documentstyle[11pt]{article} % % PAGE LAYOUT: % \textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset -0.35in \topmargin 0.305in \oddsidemargin +0.35in \evensidemargin -0.35in %\renewcommand{\rmdefault}{ptm} % to use Times font \long\def\TITLE#1{{\Large{\bf#1}}}\long\def\AUTHORS#1{ #1\\[3mm]} \long\def\AFFILIATION#1#2{$^{#1}\,$ #2\\} \begin{document} {\small \it Nuclear Physics in Astrophysics 8, NPA8: 18-23 June 2017, Catania, Italy} \vspace{12pt} \thispagestyle{empty} \begin{center} %%% %%% Title goes here. %%% \TITLE{Measurements Of Stellar And Big-Bang Nucleosynthesis Reactions Using Inertially-Confined Plasmas }\\[3mm] %%% %%% Authors and affiliations are next. The presenter should be %%% underlined as shown below. %%% \AUTHORS{A.B. Zylstra$^1$, H.W. Herrmann$^1$, M. Gatu Johnson$^2$, Y.H. Kim$^1$, J.A. Frenje$^2$, G. Hale$^1$, C.K. Li$^2$, M. Rubery$^3$, M. Paris$^1$, A. Bacher$^4$, C.R. Brune$^5$, D.T. Casey$^7$, C. Forrest$^6$, V. Yu. Glebov$^6$, R. Janezic$^6$, D. McNabb$^7$, A. Nikroo$^7$, J. Pino$^7$, T.C. Sangster$^6$, D.B. Sayre$^7$, F.H. S{\'e}guin$^2$, H. Sio$^2$, C. Stoeckl$^6$, R.D. Petrasso$^2$ } %%% {\small \it \AFFILIATION{1}{Los Alamos National Laboratory, Los Alamos, NM 87544 USA} \AFFILIATION{2}{Massachusetts Institute of Technology, Cambridge, MA 02139, USA} \AFFILIATION{3}{Plasma Physics Dept, AWE plc, Reading RG7 7PR, UK} \AFFILIATION{4}{Indiana University, Bloomington, IN 47405, USA} \AFFILIATION{5}{Ohio University, Athens, OH 45701, USA} \AFFILIATION{6}{Laboratory for Laser Energetics, University of Rochester, Rochester, NY 14623, USA} \AFFILIATION{7}{Lawrence Livermore National Laboratory, Livermore, CA 94550, USA} } %%% \vspace{12pt} % Do not modify % Enter contact e-mail address here. \centerline{Contact email: {\it zylstra@lanl.gov}} \vspace{18pt} % Do not modify \end{center} %%% %%% Abstract proper starts here. %%% The $^3$He+$^3$He, T+$^3$He, and p+D reactions directly relevant to either Stellar or Big-Bang Nucleosynthesis (BBN) have been studied at the OMEGA laser facility using inertially-confined plasmas. These high-temperature plasmas are created using shock-driven exploding pusher' implosions. The advantage of using these plasmas is that they better mimic astrophysical systems than cold-target accelerator experiments. A new measured S-factor for the T($^3$He,$\gamma$)$^6$Li reaction rules out an anomalously-high $^6$Li production during the Big Bang as an explanation to the high observed values in metal poor first generation stars. Our value is also inconsistent with values used in previous BBN calculations [1]. In a second experiment, proton spectra from the $^3$He+$^3$He and T+$^3$He reactions are used to constrain nuclear R-matrix modeling. The spectral shapes disagree with R-matrix calculations using coefficients derived from fits to T+T data at higher or lower center-of-mass energy. Finally, recent experiments have probed the p+D reaction for the first time in a plasma; this reaction is relevant to energy production in protostars, brown dwarfs, and at higher CM energies, to BBN. The first plasma data is consistent with previous accelerator experiments at $E_{cm} \sim 16$ keV, work is ongoing to further reduce our experimental uncertainties. \bigskip {\small \noindent [1] A.B. Zylstra et al., Phys. Rev. Lett. 117, 035002 (2016). } %%% %%% End of abstract. %%% \end{document}
Speaker: Dr Alex Zylstra (Los Alamos National Laboratory)
• 10:20
Nuclear Astrophysics at ELI-NP: the ELISSA prototype tested 20m
The Extreme Light Infrastructure-Nuclear Physics (ELI-NP) facility, under construction in Magurele near Bucharest in Romania, will provide high-intensity and high-resolution gamma ray beams that can be used to address hotly debated problems in nuclear astrophysics, such as the accurate measurements of the cross sections of the 24Mg( ,)20Ne reaction, that is funda- mental to determine the effective rate of 28Si destruction right before the core collapse and the subsequent supernova explosion [1], and other photo-dissociation processes relevant to stellar evolution and nucleosynthesis [2]. For this purpose, a silicon strip detector array (named ELISSA, acronym for Extreme Light In- frastructure Silicon Strip Array) will be realized in a common effort by ELI-NP and INFN-LNS (Catania, Italy), in order to measure excitation functions and angular distributions over a wide energy and angular range. According to our simulations, the final design of ELISSA will be a very compact barrel configuration, leaving open the possibility in the future to pair a neutron detector with the array. The kinematical identification will allow to separate the reaction of interest from others thanks to the good expected angular and energy resolutions. A prototype of ELISSA was built and tested at Laboratori Nazionali del Sud (INFN-LNS) in Catania with the support of ELI-NP. In this occasion, we have carried out experiments with alpha sources and with a 11 MeV 7Li beam. We used X3 and QQQ3 silicon-strip position sen- sitive detectors manufactured by Micron Semiconductor ltd. Thanks to our approach, the first results of those tests show up a very good energy resolution (better than 1%) and very good position resolution, of the order of 1 mm. At very low energies, below 1 MeV, a worse position resolution is found, of the order of 5 mm, but still good enough for the measurement of angular distribution and the kinematical identification of the reactions induced on the target by gamma beams. Moreover, a threshold of 150 keV can be easily achieved with no cooling. We will discuss technical details of the detector and present results regarding Monte Carlo simulation, energy resolution and detection thresholds of ELISSA, the physical cases to be investigated. To sum up, these tests allow us to say that the X3 detectors, as well the standard QQQ3 detec- tors, are perfectly suited for nuclear astrophysics studies with ELISSA. In particular, ELISSA will allow us to determine a much more accurate cross section for the 24Mg photodissociation to be used in nuclear reaction network calculations to improve the knowledge of the pre-supernova chemical composition.
Speaker: Giovanni Luca Guardo (LNS)
• 10:40
Monte Carlo simulation of photonuclear reactions of astrophysical interest with intense gamma sources 20m
Monte Carlo simulation of photonuclear reactions of astrophysical interest with intense gamma sources
• 11:00 11:20
Coffee break 20m Sala conferenze

### Sala conferenze

#### Laboratori Nazionali del Sud

Via S. Sofia 62 I-95123 Catania Italy
• 11:20 13:30
RIBs in nuclear astrophysics 2 Sala conferenze

### Sala conferenze

#### Laboratori Nazionali del Sud

Via S. Sofia 62 I-95123 Catania Italy
• 11:20
Studies of X-ray burst reactions with radioactive ion beams from RESOLUT 30m
% % Nuclear Physics in Astrophysics 8 template for abstract % % Format: LaTeX2e. % % Rename this file to name.tex, where name' is the family name % of the first author, and edit it to produce your abstract. % \documentstyle[11pt]{article} % % PAGE LAYOUT: % \textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset -0.35in \topmargin 0.305in \oddsidemargin +0.35in \evensidemargin -0.35in %\renewcommand{\rmdefault}{ptm} % to use Times font \long\def\TITLE#1{{\Large{\bf#1}}}\long\def\AUTHORS#1{ #1\\[3mm]} \long\def\AFFILIATION#1#2{$^{#1}\,$ #2\\} \begin{document} {\small \it Nuclear Physics in Astrophysics 8, NPA8: 18-23 June 2017, Catania, Italy} \vspace{12pt} \thispagestyle{empty} \begin{center} %%% %%% Title goes here. %%% \TITLE{Studies of X-ray burst reactions with radioactive ion beams from RESOLUT}\\[3mm] %%% %%% Authors and affiliations are next. The presenter should be %%% underlined as shown below. %%% \AUTHORS{J. C. Blackmon$^{1}$, M. Anastasiou$^{2}$, L.~T.~Baby$^{2}$, J.~Baker$^{2}$, J. Belarge$^{2}$, K.~Colbert$^{3}$, C.~M.~Deibel$^1$, H.~E.~Gardiner$^1$, D.~L.~Gay$^3$, E.~Good$^1$, P.~H\"oflich$^2$, A.~A.~Hood$^1$, K.~Joerres$^1$, N.~Keely$^4$, S.~A.~Kuvin$^2$, J. Lai$^1$, A.~Laminack$^1$, L.~E.~Linhardt$^1$, J.~Lighthall$^1$, K.~T.~Macon$^1$, E. Need$^1$, N. Quails$^4$, B.~C.~Rasco$^1$, N. Rijal$^2$, A. Volya$^2$, I. Wiedenh\"over$^2$} %%% {\small \it \AFFILIATION{1}{Louisiana State University, Baton Rouge, LA 70803 USA} \AFFILIATION{2}{Florida State University, Tallahassee, FL 32306 USA} \AFFILIATION{3}{University of North Florida, Jacksonville, FL 32224 USA} \AFFILIATION{4}{National Center for Nuclear Research, Otwock, Poland} } %%% \vspace{12pt} % Do not modify % Enter contact e-mail address here. \centerline{Contact email: {\it blackmon@lsu.edu}} \vspace{18pt} % Do not modify \end{center} %%% %%% Abstract proper starts here. %%% X-ray bursts are the most common stellar explosions in the Galaxy, occurring in binary systems when hydrogen-rich matter from a main-sequence star accretes onto a neutron star and ignites in a thermonuclear runaway. Simulations of these events show that particular nuclear reactions involving proton-rich radioactive nuclei have a direct impact on energy generation, nucleosynthesis, and astronomical observables. [1,2] The rates of many of these reactions have large uncertainties due experimental challenges in studying the properties of short-lived nuclei, which negatively impacts our understanding of these systems. Some of the most important reactions that influence the X-ray burst light curve involve the transition from the hot CNO cycle to the $\alpha p$ and $rp$ processes. We have been studying these reactions using in-flight radioactive ion beams of $^{17}$F, $^{18}$Ne and $^{19}$Ne from the RESOLUT facility at the Fox Superconducting Accelerator Laboratory at Florida State University. The relatively low intensity of the available beams has required the development of sensitive experimental techniques. Direct measurements of $(\alpha,p)$ reactions were performed using the Array for Nuclear Astrophysics and Structure with Exotic Nuclei (ANASEN). ANASEN is an active gas target detector that allows simultaneous measurement of an excitation function for scattering and reactions over a range of energies with good center-of-mass energy resolution. [3] Studies of the $(d,n)$ proton transfer reaction were performed using an array of detectors including the RESONEUT neutron detector array and a position-sensitive gas ionization detector [4]. We will present an overview of recent measurements using ANASEN and RESONEUT and preliminary results that are of interest for understanding X-ray bursts. This work was supported by the U.S. Department of Energy, Office of Science under Grants No. DE-FG02-96ER40978 and No. DE-FG02-02ER41220, and the U.S. National Science Foundation under awards PHY-1401574, PHY-1064819, and PHY-1126345. \bigskip {\small \noindent [1] A. Parikh {\it et al.} Astrophys. J. Supp. Ser. {\bf 178}, 110 (2008); \noindent [2] R. Cyburt {\it et al.}, Astrophys. J. {\bf 830}, 55 (2016); \noindent [3] E.~Koshchiy {\it et al.}, submitted to Nucl. Instrum. Methods Phys. Res. A; \noindent [4] J.~Belarge {\it et al.}, Phys. Rev. Lett. {\bf 117}, 182701 (2016). } %%% %%% End of abstract. %%% \end{document}
Speaker: Jeffery Blackmon (Louisiana State University)
• 11:50
Improved experimental determination of the branching ratio for beta-delayed alpha decay of N-16 20m
While the C-12(alpha,gamma)O-16 reaction plays a central role in nuclear astrophysics, the cross section is too small at the energies relevant to stellar helium burning to be directly measured in the laboratory. The beta-delayed alpha spectrum of N-16 can be used to constrain the astrophysical S-factor, but with this approach the S-factor becomes strongly correlated with the assumed alpha-decay branching ratio. Using two different experimental techniques, we have obtained consistent values for this branching ratio which, however, deviate significantly from the accepted value. Here, we report on our findings and discuss the implications for the determination of the astrophysical S-factor of the C-12(alpha,gamma)O-16 reaction.
Speaker: Dr Oliver Kirsebom (Department of Physics and Astronomy, Aarhus University)
• 12:10
Cousin of the Hoyle state: Observation of a narrow resonance above 13N+2p threshold 20m
The existence of the Hoyle state is crucial for the nucleosynthesis of the chemical elements heavier than lithium. This state has been the subject of many theoretical studies and philosophical discussions (anthropic principle). The existence of this remarkable state could be explained by the Ikeda conjecture [1,2]. The latter can be formulated simply: The coupling to a nearby cluster decay channel induces cluster correlations in nuclear wave functions. The Hoyle state resides just above the threshold for decay into 8Be and an alpha particle. The Ikeda conjecture implies that the Hoyle state should have an alpha cluster structure. We performed a study of the unbound nucleus 15F. Intense and pure radioactive beam of 14O, produced at GANIL (France) with the SPIRAL1 facility, was used to study the 15F low-lying states [3]. Exploiting resonant elastic scattering in inverse kinematics with a thick target, the resonance corresponding to the second excited state (J=1/2-) was measured with a width of only 36(5)(14) keV. This state is precisely located just above the two-proton threshold. The structure of this narrow above-barrier state in a nucleus located two neutrons beyond the proton drip line was investigated using the Gamow Shell Model in the coupled channel representation with a 12C core and three valence protons. It is found that it is an almost pure wave function of two-proton cluster. [1] K. Ikeda et al., Prog. Theor. Phys. Suppl., Extra Number, 464(1968). [2] J. Okołowicz, M. Płoszajczak and W. Nazarewicz. Progress of Theoretical Physics Supplement 196, 230 (2012). 65, 100 [3] F. de Grancey et al., Physics Letters B758 (2016)26–31
Speaker: Dr François de Oliveira Santos (GANIL)
• 12:30
Key Resonances in $^35$Ar and their importance for determining the origin of presolar grains 20m
% % Nuclear Physics in Astrophysics 8 template for abstract % % Format: LaTeX2e. % % Rename this file to name.tex, where name' is the family name % of the first author, and edit it to produce your abstract. % \documentstyle[11pt]{article} % % PAGE LAYOUT: % \textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset -0.35in \topmargin 0.305in \oddsidemargin +0.35in \evensidemargin -0.35in %\renewcommand{\rmdefault}{ptm} % to use Times font \long\def\TITLE#1{{\Large{\bf#1}}}\long\def\AUTHORS#1{ #1\\[3mm]} \long\def\AFFILIATION#1#2{$^{#1}\,$ #2\\} \begin{document} {\small \it Nuclear Physics in Astrophysics 8, NPA8: 18-23 June 2017, Catania, Italy} \vspace{12pt} \thispagestyle{empty} \begin{center} %%% %%% Title goes here. %%% \TITLE{Key Resonances in $^{35}$Ar and their importance for determining the origin of presolar grains }\\[3mm] %%% %%% Authors and affiliations are next. The presenter should be %%% underlined as shown below. %%% \AUTHORS{R.S. Ilieva$^{1}$, G. Lotay$^1$, D. Seweryniak$^2$, K. Auranen$^2$, R.S. Wilkinson$^{1}$, S. Hallam$^{1}$, M.P. Carpenter$^2$, R.V.F. Janssens$^2$, T. Lauritsen$^2$, R. Talwar$^2$, S. Zhu$^2$} %%% {\small \it \AFFILIATION{1}{Department of Physics, University of Surrey, Guildford, Surrey, GU2 7XH, UK} \AFFILIATION{2}{Argonne National Laboratory, Argonne, Illinois 60439, USA} } %%% \vspace{12pt} % Do not modify % Enter contact e-mail address here. \centerline{Contact email: {\it r.ilieva@surrey.ac.uk}} \vspace{18pt} % Do not modify \end{center} %%% %%% Abstract proper starts here. %%% Classical novae are among the most common explosive stellar events and therefore provide a wealth of astronomical observational data. Presolar grains are microscopic grains embedded within primitive meteorites which provide a snapshot of nucleosynthesis within a specific astrophysical site. As such, they can be used to investigate distributions of elemental abundances and allow a comparison between the predictions of theoretical models and astronomical observations. However, without accurately classifying their specific stellar origin, interpreting data from presolar grains can be difficult, as novae grain signatures are ambiguous with those from supernovae. Sulphur abundances are a key part of accurately classifying presolar grains as being of nova origin. Yet, due to large uncertainties in the nuclear processes involved in classical novae, a number of key aspects of nova nucleosynthesis remain unclear. Therefore, it is essential to obtain detailed knowledge of the nuclear reactions that are responsible for isotopic abundance signatures in presolar grains. A detailed theoretical study by Iliadis and \textit{et al.} [1] investigated the effect of nuclear reaction rate uncertainties in novae nucleosynthesis and highlighted the $^{34}$Cl$(p, \gamma)^{35}$Ar as one of only a handful of reactions to significantly affect the final production of $^{34}$S produced in ONe novae. Constraining this reaction rate is vital for the classification of presolar grains, as the $^{32}$S/$^{34}$S ratio is a key identifier of nova origins. In these environments, the $^{34}$Cl$(p, \gamma)^{35}$Ar reaction is expected to be dominated by resonant capture to excited states above the proton threshold in $^{35}$Ar. However, only limited experimental information exists on the properties of the states observed in this energy range [2]. A detailed $\gamma$-ray spectroscopy study of $^{35}$Ar was performed using the Digital Gammasphere array in combination with the Argonne Fragment Mass Analyser in order to study resonant states for the $^{34}$Cl$(p, \gamma)^{35}$Ar reaction. Excited levels in $^{35}$Ar have been identified and their spins and parities constrained, and their astrophysical implications will be discussed. \bigskip {\small \noindent [1] C. Iliadis \textit{et al.}, Astrophys. J Suppl. Ser. {\bf{142}}, 105 (2002) ; \noindent [2] C. Fry\textit{et al.}, Phys. Rev. C {\bf{91}}, 015803 (2015) } %%% %%% End of abstract. %%% \end{document}
Speaker: Ms Ralitsa Ilieva (University of Surrey)
• 12:50
Observation of the 2+ rotational excitation of the Hoyle state 20m
We present the first clear observation of the 2+ rotational excitation of the Hoyle state in a beta decay experiment. Coincident detection of β-3α particles from the cascade 12N(β)12C(α1)8Be(α2)α3 have been used to obtain β-α1 angular correlation, which then has been used to determine the strength of the 2+ state relative to that of the 0+ in the 9-12 MeV energy region. The experiment has been performed at the IGISOL facility at JYFL, Jyväskylä, Finland. This second 2+ state of the 12C nucleus is of great importance to nuclear astrophysics reaction rate calculations and also to nuclear cluster structure studies. The triple-α process, which is responsible for 12C production, primarily proceeds through a resonance in the 12C nucleus, famously known as the Hoyle state. The cluster nature of the Hoyle state allows the formation of a rotational band built upon it. The first member of the band is thought to be in the 9-11 MeV region, with Jπ=2+ [1-4], with the most recent data indicating an energy of 10.03 MeV [5]. Further knowledge of this state would help not only to understand the debated structure of the 12C nucleus in the Hoyle state, but also to determine the high-temperature (> 1 GK) reaction rate of the triple-α process more precisely [6,7]. The precise evaluation of the rate of this reaction is required to be able to understand the final stages of stellar nucleosynthesis and the elemental abundances in the universe. Due to the significance of the resonance, a reconciliation of the data from different available probes is highly desirable. We therefore, for the first time, present a clean identification of the 2+ resonance populated in beta decay through application of the novel technique of beta-triple-alpha coincidence studies. We further discuss the impact of the resonance on high-temperature astrophysical scenarios. [1] H .O. U. Fynbo, C. Aa. Diget, Hyperfine interactions 223, 1-3 (2014); [2] S. Hyldegaard et al., Phys. Rev. C 81, 024303 (2010); [3] M. Itoh et al., Phys. Rev. C 84, 054308 (2011); [4] M. Freer et al., Phys. Rev. C 80, 041303(R) (2009); [5] W. R. Zimmerman et al., Phys. Rev. Lett. 110, 152502 (2013); [6] C. Angulo et al., Nucl. Phys. A 656, 3 (1999); [7] R. H. Cyburt et al., Astrophys. J. Suppl. Ser. 189, 240 (2010).
Speaker: Ms Ruchi Garg (University of York)
• 13:10
Measurement of 21Na(α,p)24Mg cross section for the study of 44Ti production in supernovae. 20m
While core collapse supernovae have long captured the attention of physicists and astronomers, surprisingly little is currently known about the nature of the explosion mechanism. This is due to the complexity of the explosion, the large computational requirements for even 2D simulations, and the lack of precise nuclear physics inputs to these models. One of the few methods by which this explosion mechanism might be studied is through a comparison of the amount of 44Ti observed by space based γ-ray telescopes and the amount predicted to have been generated during the explosion. For these comparisons between observations and models to be made, however, more precise nuclear physics inputs are required. The reaction 21Na(α,p)24Mg has been identified as one of the key reactions affecting the 44Ti mass fraction by factors of 10 or more. There are currently no published data on this reaction. A direct experimental measurement of the 21Na(α,p)24Mg cross section has been carried out at TRIUMF, Canada. This experiment utilised the TUDA facility at ISAC-I. The 21Na radioactive beam, at high intensity, impinged on a 2cm wide gas target, containing 100 torr of 4He. A downstream silicon array, consisting of a dE-E telescope, detected the reaction protons. An upstream silicon array measured beam back-scattered from a Au foil located at the entrance of the gas target, for normalisation. Data were collected at four laboratory energies covering Ecm=3.2-2.5 MeV, which is approximately the top half of the 2GK Gamow Window. Preliminary analysis results will be presented, along with details of the experimental challenges encountered and the steps taken to overcome them.
Speaker: Dr Alison Laird (University of York)
• 13:30 14:30
Lunch 1h Sala conferenze

### Sala conferenze

#### Laboratori Nazionali del Sud

Via S. Sofia 62 I-95123 Catania Italy
• 14:30 19:30
Social excursion Siracusa

#### Siracusa

• Thursday, 22 June
• 08:30 10:10
Stellar models Aula magna (Dipartimento di Fisica e Astronomia)

### Aula magna

#### Dipartimento di Fisica e Astronomia

Via S. Sofia 64 I-95123 Catania Italy
• 08:30
Hydrostatic and Explosive Nucleosynthesis in Massive Stars 30m Aula magna

### Aula magna

#### Dipartimento di Fisica e Astronomia

Via S. Sofia 64 I-95123 Catania Italy
Speaker: Dr MARCO LIMONGI (INAF-OAR)
• 09:00
s process in massive stars: theoretical predictions and nuclear and stellar uncertainties 30m Aula magna

### Aula magna

#### Dipartimento di Fisica e Astronomia

After introducing the slow neutron capture process in massive stars, the so-called weak s process, I will present recent theoretical predictions for the weak s process covering a wide range of initial masses and metallicities. I will in particular discuss the strong effects of rotation at low metallicities and how they boost the weak s process. I will then compare the predictions to observations and discuss the key nuclear and stellar uncertainties involved. I will end with conclusions and future outlook.
Speaker: Dr Raphael Hirschi (Keele University)
• 09:50
A unique mechanism to account for well known peculiarities of AGB star nucleosynthesis 20m Aula magna

### Aula magna

#### Dipartimento di Fisica e Astronomia

We present here the application of a model for a mass circulation mechanism in between radia- tive layers and the base of the convective envelope of low mass AGB stars, aimed at studying peculiar aspects of their nucleosynthesis. Until recently the observational evidence that s-process elements from Sr to Pb are produced by stars ascending the second giant branch could not be explained by self-consistent models, forcing researchers to extensive parameterizations. The cru- cial point is to understand how protons can be injected from the envelope into the He-rich layers, yielding the formation of 13C and then the activation of the 13C(α,n)16O reaction. On the other hand, a mass circulation mechanism in between the H-burning shell and the convective envelope is belived to account for the peculiar abundances of light nuclei (from 3He to 26Mg) observed in low mass AGB stars [1]. Also in this case, despite more than twenty years of studies, we still have not achieved a final statement on the physical process responsible for the mass transportation. The mixing scheme we present is based on a previously suggested magnetic-buoyancy process [2]. We show the ”magnetic” mass transport to account adequately for both the formation of the main neutron source for s-processing in low mass AGBs [3] and the peculiar abundances of light nuclei observed in these stars. In particular our analysis results are focused on addressing the constrains to AGB nucleosynthesis coming from the isotopic composition of presolar grains recovered in meteorites [4,5]. We find that (i) n-captures driven by the magnetically-induced mixing can account for the isotopic abundance ratios of s-elements recorded in presolar SiC grains as well as (ii) the most extreme levels of 18O depletion and high concentration of 26Mg (from the decay of 26Al) shown by corundum (Al2O3) grains. [1] G. J.Wasserburg, A. I. Boothroyd, I.-J. Sackmann, ApJ 447 L37 (1995); [2] M. C. Nucci & M. Busso ApJ, 787 141 (2014); [3] O. Trippella, M. Busso, S. Palmerini, et. al., ApJ 818 125 (2016); [4] S. Palmerini, O. Trippella, M. Busso, MNRAS, in press (2017); [4] S. Palmerini, O. Trippella, M. Busso, et al. GCA, submitted.
Speaker: Sara Palmerini (PG)
• 10:10 10:30
Coffee break 20m Aula magna (Dipartimento di Fisica e Astronomia)

### Aula magna

#### Dipartimento di Fisica e Astronomia

• 10:30 13:00
Special session: celebrating Claudio Spitaleri Aula magna (Dipartimento di Fisica e Astronomia)

### Aula magna

#### Dipartimento di Fisica e Astronomia

Via S. Sofia 64 I-95123 Catania Italy
• 10:30
The origins of the THM 15m Aula magna

### Aula magna

#### Dipartimento di Fisica e Astronomia

Via S. Sofia 64 I-95123 Catania Italy
• 10:45
TBD 15m Aula magna

### Aula magna

#### Dipartimento di Fisica e Astronomia

Via S. Sofia 64 I-95123 Catania Italy
Speaker: Silvio Cherubini (LNS)
• 11:00
And so it all began: Personal memories of the man behind the scientist 15m Aula magna

### Aula magna

#### Dipartimento di Fisica e Astronomia

Via S. Sofia 64 I-95123 Catania Italy
At the time I began my scientific career as a PhD student under Prof Claudio Spitaleri’s supervision, the Trojan Horse Method was still in its infancy. Like with any new-born idea, it took time and effort and passion to plant the early seeds that would eventually develop into a now well-established method in nuclear astrophysics research. In this talk I will offer my own recollection of those early years as a personal tribute to Claudio's unique mix of human traits that shaped our professional relationship for decades to come.
Speaker: Prof. Marialuisa Aliotta (University of Edinburgh)
• 11:15
Theory of the Trojan-Horse Method - From the original idea to actual applications 15m Aula magna

### Aula magna

#### Dipartimento di Fisica e Astronomia

Breakup reactions were proposed in 1986 by Gerhard Baur as an indirect method to investigate low-energy charged-particle reactions relevant for nuclear astrophysics [1]. This so-called 'Trojan-Horse method' (THM) allows to extract cross sections of two-particle reactions from suitable transfer reactions with three particles in the final state using quasifree scattering conditions. A specific feature of the approach is the suppression of the Coulomb barrier effect that causes a strong reduction of the cross section of astrophysical reactions at low energies. The THM is applicable to general rearrangement reactions in contrast to other indirect techniques such as the Coulomb dissociation (CD) method or asymptotic normalization coefficient (ANC) method, which aim at radiative capture reactions. The analysis of dedicated laboratory experiments using the THM requires the application of nuclear reaction theory. In this contribution, the development of the theoretical description is presented starting from the early ideas with simple approximations, e.g., a modified plane-wave impulse approximation (PWIA) that allowed to factorize the THM cross section as a product of a kinematic factor, a momentum distribution and a half-off-shell two-body cross section. Different applications are considered, in particular, elastic scattering, non-resonant and resonant reactions. Suggestions for possible improvements in the future development of the theory are given. [1] G. Baur, Phys. Lett. B 178, 135 (1986).
Speaker: Dr Stefan Typel (IKP, Technische Universität Darmstadt)
• 11:30
Clustering of light nuclei and electron screening in astrophysical environments (EPS Invited Speaker) 15m Aula magna

### Aula magna

#### Dipartimento di Fisica e Astronomia

Accurate measurements of nuclear reactions of astrophysical interest within, or close to, the Gamow peak show evidence of an unexpected effect attributed to the presence of atomic electrons in the target. The experiments need to include an effective “screening” potential to explain the enhancement of the cross sections at the lowest measurable energies. Despite various theoretical studies conducted over the past 20 years and numerous experimental measurements, a theory has not yet been found that can explain the cause of the exceedingly high values of the screening potential needed to explain the data. In this talk I will show that instead of an atomic physics solution of the “electron screening puzzle”, the reason for the large screening potential values is in fact due to clusterization effects in nuclear reactions, in particular for reaction involving light nuclei.
Speaker: Prof. Carlos Bertulani (Texas A&amp;M University-Commerce)
• 11:45
Coulomb dissociation - another Trojan Horse 15m Aula magna

### Aula magna

#### Dipartimento di Fisica e Astronomia

Via S. Sofia 64 I-95123 Catania Italy
I start with my experience for the quasi-free process, which is on the 1H(d,2He)n reaction, where 2He denotes a system of two protons in their unbound singlet S state. The data taken at Saturne in late 1980s were analyzed with plane-wave impulse approximation. The tensor analyzing powers and even the absolute magnitudes of the differential cross sections have been successfully explained. That was my surprise, because nucleon rearrangement reactions are not always described by such a simple treatment. The second time when I encountered such unexpected (to my view) success is the occasion when I heard a talk by Prof. Spitaleri on the Trojan Hourse determination of astrophysical reactions. The process is a “quasi-free reaction” leaving a three-body final state with a particle-unbound subsystem. A remarkable agreement between the excitation functions of the original and extracted reaction of interest was demonstrated, at least, in that case, for their relative energy-dependence. It should be noted that the incident energy is not very high and complicated processes could contribute. These observations lead me a “feeling”: the quasi-free mechanism can naturally find a way to particle-unbound final state, while population of discrete bound-states requires more kinematically restricted conditions and may allow for complicated mechanism to be involved. That is only my prejudice, but we should thank this favorable situation. The Trojan Hourse method can indirectly access particle rearrangement reactions of astrophysical interest. Another indirect method that can study radiative capture, often of importance in nucleosynthesis, is the Coulomb dissociation. I conducted several experiments in the period when Prof. Spitaleri vigorously studied and were establishing the Torojan Hourse method. Coulomb dissociation, that is inelastic scattering exciting a nucleus to its unbound state, is often explained in terms of virtual photons created when the two colliding nuclei come close to each other. In fast collisions, the breakup process involves a single photon and can therefore be understood as a Trojan Horse reaction, where the photon serves as a "soldier". Several radiative capture reactions of astrophysical interest have been studied. Especially with fast radioactive-isotope (RI) beams, processes involved in explosive nuclear burning, such as the hot CNO cycle and rp-process, could be accessed.
Speaker: Dr Tohru Motobayashi (RIKEN Nishina Center)
• 12:00
Subtilities in Stars: Indirect Evidence of Mixing Married to Indirect Nuclear Physics Methods 15m Aula magna

### Aula magna

#### Dipartimento di Fisica e Astronomia

Via S. Sofia 64 I-95123 Catania Italy
Speaker: Maurizio Busso (PG)
• 12:15
"Other" indirect methods for Nuclear Astrophysics 15m Aula magna

### Aula magna

#### Dipartimento di Fisica e Astronomia

Via S. Sofia 64 I-95123 Catania Italy
In the house of Trojan Horse Method (THM), I will say a few words about "other" indirect methods we use in Nuclear Physics for Astrophysics. In particular those using Rare Ion Beams that can be used to evaluate radiative proton capture reactions. I addition a few words about work done with the Professore we celebrate today. With a proposal, and some results with TECSA, for a simple method to produce and use isomeric beam of 26mAl.
Speaker: Dr Livius Trache (IFIN-HH Bucharest)
• 12:45
Alpha-cluster structure populated in the resonance reactions induced by rare beams 15m Aula magna

### Aula magna

#### Dipartimento di Fisica e Astronomia

Via S. Sofia 64 I-95123 Catania Italy
Alpha-cluster structure populated in the resonance reactions induced by rare beams V.Z. Goldberg, G.V. Rogachev Cyclotron Institute, Texas A&M University, College Station, TX 77843, USA The alpha clusterization manifests itself in remarkable and exotic structures in atomic nuclei. In particular, quasi rotational bands of levels with alternative parities and large alpha cluster reduced widths are well known in the light 4N nuclei (like 8Be, 12C, 16O...). The importance of this nuclear structure in astrophysics is also well recognized. Even if astrophysical reactions involving helium do not proceed through the strong α-cluster states, these states provide α width to the states that are closer to the region of astrophysical interest through configuration mixing. While the phenomenon is known, a detailed explanation in the framework of the N-N interaction is absent [1,2]. The scarce experimental data on the single particle properties of the cluster states is partly responsible for this situation. Indeed, the α decay threshold is much lower than the nucleon decay in 4N nuclei, and, therefore, nucleon decays cannot be practically observed from the members of the cluster bands. In N≠Z nuclei, the nucleon decay threshold is close to that for α particle, and the penetrability factors do not inhibit the nucleon decay from the states in question. It is also possible to use mirror resonance reactions and apply the powerful approach of isospin symmetry to the investigations involving N≠Z nuclei. Of course, such studies involve unstable (Z>N) nuclei. Therefore, the experiments are difficult and need a new technique to study resonance reactions. The first measurements of the resonance reactions involving a pair of N≠Z nuclei were made in Ref. [3]. Since then, a few attempts to develop the field were made (see [4,5]]. I will review the history, the problems, and the prospective of these studies. References 1. P.Navratil, J.P.Vary, B.R.Barrett Phys.Rev.Lett. 84,5729 (2000) 2. M.L.Avila, G.V.Rogachev, V.Z.Goldberg et al., Phys. Rev. C 90, 024327 (2014) 3. V.Z.Goldberg, G.V.Rogachev... C.Spitaleri et al., Phys.Rev. C 69, 024602 (2004) 4. C.Fu, V.Z.Goldberg, G.V.Rogachev et al., Phys.Rev. C 77, 064314 (2008) 5. E.D.Johnson, G.V.Rogachev, V.Z.Goldberg et al., J.Phys.:Conf.Ser. 205, 012011 (2010)
Speaker: Dr Vladilen Goldberg (Cyclotron Institute, Texas A&M University, College Station, Texas, USA)
• 13:30 14:30
Lunch 1h Aula magna (Dipartimento di Fisica e Astronomia)

### Aula magna

#### Dipartimento di Fisica e Astronomia

• 14:30 16:30
Indirect methods 1 Aula magna (Dipartimento di Fisica e Astronomia)

### Aula magna

#### Dipartimento di Fisica e Astronomia

Via S. Sofia 64 I-95123 Catania Italy
• 14:30
THM measurements in nuclear astrophysics: recent results and future perspectives 30m Aula magna

### Aula magna

#### Dipartimento di Fisica e Astronomia

Via S. Sofia 64 I-95123 Catania Italy
Experimental nuclear astrophysics aims at measuring astrophysically relevant burning reaction cross sections at the corresponding Gamow energy. However, in spite of the improvements for measuring low-energy nuclear reaction cross sections, the Gamow energy region peak often remains far to be fully explored mainly in the case of charged-particles induced reactions. In such cases, both Coulomb barrier penetration and electron screening phenomena strongly affect the bare-nucleus cross section determination thus leaving extrapolation procedures as the only way for accessing the Gamow energy region. The Trojan Horse Method (THM) allows one to measure the bare-nucleus cross-section of an astrophysically relevant reaction a+x→c+C by properly selecting the quasi-free (QF) contribution of an appropriate reaction a+A→c+C+s, performed at energies well above the Coulomb barrier, where the nucleus A has a dominant x⊕s cluster configuration. Thanks to its momentum-energy prescription, THM allows to explore a wide energy window in the center of mass system a + x by only using a monoenergetic beam. Such advantage appears of great importance also in the case of nuclear reactions involving exotic nuclei or neutron induced reactions, thus justifying the recent THM application to well definite reactions involved in explosive or primordial nucleosynthesis. [1] Spitaleri C. et al., Phys. of Atomic Nuclei, 74, 1725 (2011) [2] Tribble, R. et al., Rep. Prog. Phys., 77, 106901 (2014)
Speaker: Livio Lamia (LNS)
• 15:00
Reaction production + AMS: An alternative method to study (d,alpha)26Al and (p,gamma)26Al reactions at low energies 30m Aula magna

### Aula magna

#### Dipartimento di Fisica e Astronomia

It is well known the importance in Astrophysics of the reactions regarding 26Al. This radioisotope is presented for instance, in the stars where there is H, C and Ne fusion at high temperatures; as well it can be found inside meteorites where it can be deposited or to be created in situ [1]. Considering the importance of the 26Al nuclei, in this work are presented the rst results regard- ing a campaign of measurements related with this radioisotope production, taking advantage of two dierent facilities: rstable, the radionucleus is produced by means of irradiation of silicon and magnesium targets with light particles, in order to produce (d,alpha) and (p, gamma) reactions at low energies by using a CN-Van der Graaff accelerator. Once the enrichment with 26Al was made, the targets are analyzed in an AMS machine with the aim to obtain the 26Al/27Al ratios [2]. This values can later be used to approach the cross section of 26Al directly related with the reaction used for its production. With this alternative method, it is possible to measure very acceptable small cross sections of low energy reactions, due to the typical high resolution of AMS technique. In this work are presented our preliminary results for the 28Si(d,alpha)26Al reaction cross sections around 1.5 MeV [3] as well as the first approximations for the 25Mg(p,gamma)26Al reaction cross sections below 1 MeV. [1] J. Kndlseder et. al. Astron. And Astrophys. 344 (1999) 68. [2] A. Arazi, et. al., Phys. Rev. C 74, 025802 (2006). [3] V. Araujo-Escalona et. al., J. of Phys. Conf. Ser, 730 (2016) 1-7.
Speaker: LUIS ARMANDO ACOSTA SANCHEZ (CT)
• 15:30
Cross section measurement of 14N(p,gamma)15O using the activation method 20m Aula magna

### Aula magna

#### Dipartimento di Fisica e Astronomia

% % Nuclear Physics in Astrophysics 8 template for abstract % % Format: LaTeX2e. % % Rename this file to name.tex, where name' is the family name % of the first author, and edit it to produce your abstract. % \documentstyle[11pt]{article} % % PAGE LAYOUT: % \textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset -0.35in \topmargin 0.305in \oddsidemargin +0.35in \evensidemargin -0.35in %\renewcommand{\rmdefault}{ptm} % to use Times font \long\def\TITLE#1{{\Large{\bf#1}}}\long\def\AUTHORS#1{ #1\\[3mm]} \long\def\AFFILIATION#1#2{$^{#1}\,$ #2\\} \begin{document} {\small \it Nuclear Physics in Astrophysics 8, NPA8: 18-23 June 2017, Catania, Italy} \vspace{12pt} \thispagestyle{empty} \begin{center} %%% %%% Title goes here. %%% \TITLE{Cross section measurement of $^{14}$N(p,$\gamma$)$^{15}$O using the activation method}\\[3mm] %%% %%% Authors and affiliations are next. The presenter should be %%% underlined as shown below. %%% \AUTHORS{Gy. Gy\"urky$^{1}$, T. Sz\"ucs$^1$, Z. Hal\'asz$^1$, G.G. Kiss$^1$, Zs. F\"ul\"op$^1$, L. Wagner$^2$, D. Bemmerer$^2$} %%% {\small \it \AFFILIATION{1}{Institute for Nuclear Research (MTA Atomki), P.O.Box 51, H-4001 Debrecen, Hungary} \AFFILIATION{2}{Helmholtz-Zentrum Dresden-Rossendorf, Bautzner Landstr 400, 01328 Dresden, Germany} } %%% \vspace{12pt} % Do not modify % Enter contact e-mail address here. \centerline{Contact email: {\it gyurky@atomki.mta.hu}} \vspace{18pt} % Do not modify \end{center} The radiative proton capture on $^{14}$N is the slowest, and thus the key reaction of the CNO cycle of stellar hydrogen burning. The rate of the $^{14}$N(p,$\gamma$)$^{15}$O reaction determines the efficiency of the CNO cycle and plays therefore an important role in the understanding of various astrophysical phenomena. The energy generation of massive stars, the solar composition problem and the age determination of globular clusters -- just to mention a few -- are all intimately related to the $^{14}$N(p,$\gamma$)$^{15}$O reaction [1,2]. Despite the huge experimental effort devoted to the cross section measurement of $^{14}$N(p,$\gamma$)$^{15}$O in the latest several decades [3], the precision of measured data is still not sufficient for the astrophysical models [4]. The aim of the present work is to measure the $^{14}$N(p,$\gamma$)$^{15}$O cross section in a wide energy using the activation method which was never used in the case of this reaction. The activation method provides directly the astrophysically important total cross section and the method is free from some uncertainties encountered in the conventional in-beam $\gamma$-spectroscopy experiments. The measurements are carried out at the new Tandetron accelerator of Atomki. Our experiment will provide an independent and precise dataset for this key reaction of nuclear astrophysics. In the talk details of the experiments and some preliminary results will be presented and compared with literature data. \bigskip {\small \noindent [1] F. L. Villante, Nucl. Part. Phys. Proc. \textbf{265-2ֲ66}, 132 (2015). \noindent [2] M. Wiescher \textit{et al.}, Annu. Rev. Nucl. Part. Sci. \textbf{60}, 381 (2010). \noindent [3] Q. Li et al., Phys. Rev. C \textbf{93}, 055806 (2016) and references therein. \noindent [4] E.G. Adelberger \textit{et al.}, Rev. Mod. Phys. \textbf{83}, 195 (2011). } %%% %%% End of abstract. %%% \end{document}
Speaker: Dr György Gyürky (Institute for Nuclear Research (Atomki)
• 15:50
Measurement of β-delayed protons from decay of 31Cl covering the Gamow window of 30P(p,γ)31S at typical nova temperatures 20m Aula magna

### Aula magna

#### Dipartimento di Fisica e Astronomia

The thermonuclear runaway in classical novae proceeds through radiative proton capture re- actions (p,γ) involving proton rich sd-shell nuclei close to the dripline. Many of the capture reactions at typical peak nova temperatures of 0.2-0.4 GK are dominated by resonant capture. Therefore, the key parameters in understanding the astrophysical reaction rates are the energies, decay widths and spins of these resonances. One of the bottleneck reactions in the ONe nova nucleosynthesis is the radiative proton capture 30P(p,γ)31S. In absence of intense 30P radioactive beams, the experimental efforts for finding and studying the resonances in 31S have concentrated on using a variety of indirect methods. One indirect method with high selectivity is the allowed β-decay of the 3/2+ ground state of 31Cl which populates excited states in 31S, corresponding to l = 0 resonances (Jπ = 1/2+,3/2+) and l = 2 resonances (J π = 5/2+ ). An observation, or non-observation, of β -delayed protons or γ -rays from the levels with uncertain or contradicting spin assignments [1] will help constraining the possible astrophysically important states. The previous efforts on measuring β-delayed protons from the states of astrophysical interest in 31S (Ex ∼ 100−500 keV) have not been successful for the fact that these studies suffered from the intense β-background in the setups utilizing Silicon detectors [2,3]. Recently, high statistics measurement of β -delayed γ -rays from decay of 31 Cl identified a new candidate for a resonance in the middle of the Gamow window [4]. Since the new level is seen populated in β-decay, it opens possibility for determining the proton branching ratio, which is one of the pieces of information needed for the experimental determination of the experimental value of the resonance strength. We have done a measurement of β-delayed protons from 31Cl with the newly built and commissioned AstroBox2 detector, based on Micro Pattern Gas Amplifier Detector (MPGAD) technology [5]. An intense and pure beam of 31Cl was produced with the MARS separator at the Texas A&M University, and implanted and stopped inside the gas volume of the AstroBox2 for the decay study. In this experiment we suppressed the β-background down to 100 keV, allowing background free study of β-delayed proton emitting states in 31S throughout the whole Gamow window of the 30P(p,γ)31S reaction. In this contribution we describe our setup and present the results of the experiment. [1] C. Ouellet and B. Singh, Nucl. Data Sheets 114, 209 (2013); [2] A. Kankainen et al., Eur. Phys. J. A 27, 67 (2006); [3] A. Saastamoinen et al., AIP Conf. Proc. 1409, 71 (2011); [4] M.B. Bennett et al., Phys. Rev. Lett. 116, 102502 (2016); [5] A. Saastamoinen et al. Nucl. Instrum. and Meth. in Phys. Res. B 376 (2016) 357.
Speaker: Dr Antti Saastamoinen (Cyclotron Insitute, Texas A&amp;amp;M University)
• 16:30 16:50
Coffee break 20m Aula magna (Dipartimento di Fisica e Astronomia)

### Aula magna

#### Dipartimento di Fisica e Astronomia

• 16:50 18:50
Indirect methods 2 Aula magna (Dipartimento di Fisica e Astronomia)

### Aula magna

#### Dipartimento di Fisica e Astronomia

Via S. Sofia 64 I-95123 Catania Italy
• 16:50
Study of stellar nucleosynthesis using indirect techniques 30m Aula magna

### Aula magna

#### Dipartimento di Fisica e Astronomia

% % Nuclear Physics in Astrophysics 8 template for abstract % % Format: LaTeX2e. % % Rename this file to name.tex, where name' is the family name % of the first author, and edit it to produce your abstract. % \documentstyle[11pt]{article} % % PAGE LAYOUT: % \textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset -0.35in \topmargin 0.305in \oddsidemargin +0.35in \evensidemargin -0.35in %\renewcommand{\rmdefault}{ptm} % to use Times font \long\def\TITLE#1{{\Large{\bf#1}}}\long\def\AUTHORS#1{ #1\\[3mm]} \long\def\AFFILIATION#1#2{$^{#1}\,$ #2\\} \begin{document} {\small \it Nuclear Physics in Astrophysics 8, NPA8: 18-23 June 2017, Catania, Italy} \vspace{12pt} \thispagestyle{empty} \begin{center} %%% %%% Title goes here. %%% \TITLE{Study of stellar nucleosynthesis using indirect techniques }\\[3mm] %%% %%% Authors and affiliations are next. The presenter should be %%% underlined as shown below. %%% \AUTHORS{F Hammache} %%% {\small \it \AFFILIATION{}{Institut de Physique Nucl$\'e$aire, IN2P3-CNRS, Universit$\'e$ Paris-Sud, Universit$\'e$ Paris-Saclay, 91406 Orsay, France} } %%% \vspace{12pt} % Do not modify % Enter contact e-mail address here. \centerline{Contact email: {\it hammache@ipno.in2p3.fr}} \vspace{18pt} % Do not modify \end{center} %%% %%% Abstract proper starts here. %%% Direct measurements of nuclear reactions of astrophysical interest can be a technical challenge. Alternative experimental techniques such as transfer reactions, inelastic scattering and charge-exchange reactions offer the possibility to study these reactions by using stable or radioactive beams. In this context, an overview of recent experiments that have been carried out in Orsay using these indirect techniques will be given. The experiments concern the study of key reactions occurring in massive stars and novae. \bigskip {\small \end{document}
Speaker: Dr Faïrouz Hammache (IPN-Orsay)
• 17:20
Measurements of the 20Ne+4He resonant elastic scattering for characterization of the 24Mg states at relevant excitations for carbon - carbon burning process 30m Aula magna

### Aula magna

#### Dipartimento di Fisica e Astronomia

Detailed knowledge on complex spectroscopy of the $^{24}$Mg nucleus at excitation energies between 14 and 19 MeV has large impact on understanding of clustering in nuclei and on carbon - carbon burning, the $^{12}$C+$^{12}$C fusion, in massive stars. The $^{12}$C+$^{12}$C and $^{16}$O+$^{8}$Be cluster structures (threshold energies are 13.9 and 14.1 MeV respectively) become active in this energy region mixing with already strong $^{20}$Ne+$^{4}$He clustering (threshold energy is 9.3 MeV). Their interplay and effects of strong $\alpha$-clustering in $^{12}$C and $^{20}$Ne lead to unique structural properties and very complex spectroscopy of the $^{24}$Mg. In this energy region are expected to exist the band heads of a number of rotational bands associated with the $^{12}$C+$^{12}$C cluster structure whose high spin members are identified at higher excitations. It is cruical to identify low spin members of these rotational bands to improve understanding of their origin. The $^{12}$C+$^{12}$C clustering has a strong effect on the C-C burning which play an essential role in many astrophysical phenomena, both quiescent and explosive. Existing data in astrophysically relevant energy range show large discrepancies in the S-factors and substantial improvements in future direct measurements are required to make further progress. Indirect experimental approach through measurements of the $^{20}$Ne+$^{4}$He resonant elastic scattering was used to search for $^{24}$Mg states which may increase C-C burning rate. Observation of the $0^+$ (or $1^-$) resonance at excitations between 15 and 18 MeV would strongly indicate enhanced reaction rate of the $^{12}$C+$^{12}$C fusion while its non-observation would imply non-resonant nature of the C-C burning, and hence its reduced contribution in many stellar phenomena. Measurements of the $^{20}$Ne+$^{4}$He excitation functions by use of the 36.07, 45.45 and 53.17 MeV $^{20}$Ne beams delivered by the PIAVE-ALPI facility of Laboratori Nazionali di Legnaro INFN and a thick $^{4}$He gas target which stops the beam in front of the detector were performed. This beam energy range corresponds to the $^{12}$C+$^{12}$C relative energy range of prime importance for astrophysics. Scattered $\alpha$-particles were detected in large area highly segmented silicon strip detector telescope built of 20 $\mu$m thick $\Delta$E SSSD and 1000 $\mu$m thick E DSSSD. Telescope was positioned at 0$^o$. Detailed measurements of the beam energy loss and beam intensity, needed for an accurate data analysis, were performed. Elastic scattering excitation functions were extracted for data between -5$^o$ and 5$^o$ and normalized to previously taken data. Large number of overlapping resonances is detected in the excitation functions. Strong contribution of the inelastic scattering to the first excited $^{20}$Ne state was observed and further analysis was performed for data free of inelastic scattering events. Using all available results on $^{24}$Mg states at these excitations, attempts to fully characterize the observed resonances in the excitation functions in terms of spin, parity, width and partial widths were done using R-matrix calculations. No clear evidence for the $0^+$ or $1^-$ state was found. Obtained results show the limitations of performed experiment and give clue for improved experiment. Complementary measurements using resonant scattering technique with the $^{20}$Ne beam and low density $^{4}$He gas target which will provide high resolution data for larger angular range were recently performed at LNL INFN and obtained data are being analysed.
Speaker: Dr Neven Soic (Rudjer Boskovic Institute Zagreb Croatia)
• 17:50
Study of the 10B(p, alpha)7Be reaction at astrophysical energy using the Trojan Horse Method 20m Aula magna

### Aula magna

Speaker: Concetta Parascandolo (NA)
• 12:20
Study of the 2H(p,gamma)3He reaction in the Big Bang nucleosynthesis energy range at LUNA 20m Aula magna

### Aula magna

#### Dipartimento di Fisica e Astronomia

Study of the 2H(p,γ)3He reaction in the Big Bang nucleosynthesis energy range at LUNA V. Mossa for the LUNA collaboration Università degli Studi di Bari and INFN, sezione di Bari Contact email: viviana.mossa@ba.infn.it The Big Bang Nucleosynthesis (BBN) describes the production of light nuclides in the first minutes of cosmic time. It started with deuterium accumulation when the Universe was cold enough to allow 2H nuclei to be survived to photo-disintegration. A primordial deuterium abundance evaluation D/H = (2.65 ± 0.07)10^−5 [1] is obtained by merging BBN calculations and CMB analysis obtained by the Planck collaboration. This value is in tension with the astronomical observations on metal-poor damped Lyman alpha systems, according to which D/H = (2.547 ± 0.033)10−5 [2]. The main source of uncertainty on standard BBN prediction of deuterium abundance is actually due to the radiative capture process 2H(p,γ)3He converting deuterium into helium, because of the poor knowledge of its S-factor at BBN energies. A measurement of this reaction cross section is thus desirable with a 3% accuracy in the energy range 10keV < Ecm < 300keV [1]. Furthermore a precise measurement of the 2H(p,γ)3He reaction cross section is crucial for testing ab-initio calculations in theoretical nuclear physics [3]. The measurement of the 2H(p,γ)3He cross section is ongoing at the Laboratory for Under- ground Nuclear Astrophysics (LUNA) taking advantage of the low background of the underground Gran Sasso Laboratories and of the experience accumulated in more than twenty years of scientific activity on precision measurements. The experiment consists of two main phases characterized by two different setups. The former provides for a windowless gas target filled with deuterium together with a 4π BGO detector. This high efficiency detector has been used for investigating the energy range between 30 keV and 260 keV, finding a continuation of the previous results obtained by the LUNA collaboration in [6], where the 2H(p,γ)3He cross section was studied in the Solar Gamow peak (2.5keV < Ecm < 22keV ). The latter phase, instead, will cover the medium-high energies (70keV < Ecm < 260keV ) using a High Purity Germanium detector (HPGe). The HPGe high resolution allows the differential cross section of the reaction to be evaluated by using the peak shape analysis. The cross section preliminary results will be shown. [1] E. Di Valentino et al., Phys. Rev. D 90 (2014) 023543; [2] R. Cooke at al., Astrophys. J. 830, 2 (2016) 148; [3] L.E. Marcucci et al., Phys. Rev. Lett. 116 (2016) 10250; [4] H. Costatini et al., Rep. Prog. Phys. 72 (2009) 086301; [5] C. Broggini et al., Ann. Rev. Nucl. Part. Sci. 60 (2010) 53; [6] C. Casella et al., Nucl. Phys.,A 706 (2002) 203.
Speaker: Viviana Mossa (Università degli Studi di Bari and INFN, sezione di Bari)
• 12:40
$^3$He($\alpha$,$\gamma$)$^7$Be cross section at high energies 20m Aula magna

### Aula magna

#### Dipartimento di Fisica e Astronomia

Via S. Sofia 64 I-95123 Catania Italy
% % Nuclear Physics in Astrophysics 8 template for abstract % % Format: LaTeX2e. % % Rename this file to name.tex, where name' is the family name % of the first author, and edit it to produce your abstract. % \documentstyle[11pt]{article} % % PAGE LAYOUT: % \textheight=9.9in \textwidth=6.3in \voffset -0.85in \hoffset -0.35in \topmargin 0.305in \oddsidemargin +0.35in \evensidemargin -0.35in %\renewcommand{\rmdefault}{ptm} % to use Times font \long\def\TITLE#1{{\Large{\bf#1}}}\long\def\AUTHORS#1{ #1\\[3mm]} \long\def\AFFILIATION#1#2{$^{#1}\,$ #2\\} \begin{document} {\small \it Nuclear Physics in Astrophysics 8, NPA8: 18-23 June 2017, Catania, Italy} \vspace{12pt} \thispagestyle{empty} \begin{center} %%% %%% Title goes here. %%% \TITLE{$^3$He($\alpha$,$\gamma$)$^7$Be cross section at high energies}\\[3mm] %%% %%% Authors and affiliations are next. The presenter should be %%% underlined as shown below. %%% \AUTHORS{\underline{T. Sz\"ucs}, Gy. Gy\"urky, Z. Hal\'asz, G.\,G. Kiss, Zs. F\"ul\"op} %%% {\small \it \AFFILIATION{}{MTA Atomki, Debrecen, Hungary} } %%% \vspace{12pt} % Do not modify % Enter contact e-mail address here. \centerline{Contact email: {\it szucs.tamas@atomki.mta.hu}} \vspace{18pt} % Do not modify \end{center} %%% %%% Abstract proper starts here. %%% The $^3$He($\alpha$,$\gamma$)$^7$Be reaction is the starting point of the ppII and ppIII reaction branches in the solar hydrogen burning, therefore its rate has sizeable impact on the solar $^7$Be and $^8$B neutrino production. Using the standard solar model [1], the flux of these neutrinos can be calculated. With the known solar parameters and reaction rates, we may have an insight into the solar core. Recently, the solar neutrino detections reached a precision of a few percent [2,3], which would allow for these investigations. However, now the precision of the nuclear physics input has to catch up to have this unique tool for precise solar core diagnostics. One of the most uncertain reaction rates is that of the $^3$He($\alpha$,$\gamma$)$^7$Be, even if many experiments have been done in the last decade clearing up some long standing issues [4,5]. Most of these reaction cross section measurements concentrated on the low energy cross sections and their precision mostly reached the limits. However, there is no experimental data above \mbox{$E_{cm} = 3.1$\,MeV}. It was suggested recently, that the R-matrix models have to be tested with higher energy datasets [6]. In addition, there are conflicting datasets for the $^6$Li(p,$\gamma$)$^7$Be reaction [7,8] having impact on the level scheme of $^7$Be. In this work the $^3$He($\alpha$,$\gamma$)$^7$Be reaction cross section was measured in a wide energy range between $E_{cm} = 2.5 - 4.4$\,MeV. A thin window gas cell target was used [9], and the cross sections were determined from the activity of the produced $^7$Be implanted into the catcher foil closing the gas cell. This method is free from any uncertainty of angular distribution effects which can be sizeable in case of resonant capture. Even if the entrance foil broadens the energy distribution of the interacting beam, thus enlarges the energy uncertainty of the measured cross sections or uncertainty of a resonance position, this effect remain small and does not to smear out any possible peak of a resonance. The final dataset will contain data points in the energy range where experimental data already exists to have possible comparisons, and extends above the proton separation energy of $^7$Be, thus it can be compared also with the $^6$Li(p,$\gamma$)$^7$Be reaction cross sections. Preliminary results will be presented and compared with literature data. \bigskip {\small \noindent [1] A. Serenelli \textit{et al.}, Phys. Rev. D \textbf{87}, 043001 (2013); \noindent [2] B. Aharmim \textit{et al.} (SNO Collaboration), Phys. Rev. C \textbf{88}, 025501 (2013); \noindent [3] G. Bellini \textit{et al.} (Borexino Collaboration), Phys. Rev. C \textbf{89}, 112007 (2014); \noindent [4] E. G. Adelberger \textit{et al.}, Rev. Mod. Phys. \textbf{70}, 1265 (1998); \noindent [5] E. G. Adelberger \textit{et al.}, Rev. Mod. Phys. \textbf{83}, 195 (2011); \noindent [6] R. J. deBoer \textit{et al.}, Phys. Rev. C \textbf{90}, 035804 (2014); \noindent [7] R. M. Prior \textit{et al.}, Phys. Rev. C \textbf{70}, 055801 (2004); \noindent [8] J. He \textit{et al.}, Phys. Lett. B \textbf{725}, 287 (2013); \noindent [9] C. Bordeanu \textit{et al.}, Nucl. Phys. A \textbf{908}, 1 (2013). } %%% %%% End of abstract. %%% \end{document}
Speaker: Dr Tamás Szücs (MTA Atomki)
• 13:00 13:20
Closing remarks Aula magna (Dipartimento di Fisica e Astronomia)

### Aula magna

#### Dipartimento di Fisica e Astronomia

Via S. Sofia 64 I-95123 Catania Italy
• 13:20 14:20
Lunch 1h Aula magna (Dipartimento di Fisica e Astronomia)