Conveners
Nuclear Astrophysics: AULA 2 (Ground Floor)
- Zsolt Fulop (ATOMKI)
- Frank Gunsing (CEA Saclay - Irfu)
Nuclear Astrophysics: AULA 2
- Zsolt Fulop (ATOMKI)
- Frank Gunsing (CEA Saclay - Irfu)
Description
Room traslazione
Stephane Goriely
(Universite Libre de Bruxelles)
04/09/2018, 14:00
One of the major issues in modern astrophysics concerns the analysis and understanding of the present composition of the Universe and its various constituting objects. Nucleosynthesis models aim to explain the origin of the
different nuclei observed in nature by identifying the possible processes able to synthesize them. Though the origin of most of the nuclides lighter than iron through the...
Dr
Gabor Gyula Kiss
(Atomki)
04/09/2018, 14:25
About 50% of the chemical elements heavier than iron are synthesized in stellar explosions, in supernovas or in neutron star mergers. After tremendous experimental and theoretical efforts and significant progress in astrophysical modeling, the origin of neither the r nor the p isotopes is fully understood. One thing is certain: improved nuclear physics knowledge is needed to describe better...
Mr
Thomas Chillery
(University of Edinburgh)
04/09/2018, 14:50
Proton-induced reactions on 6Li play an important role in nuclear astrophysics studies in relation to primordial lithium abundances. Whilst big bang nucleosynthesis theory excludes the existence of “primordial” 6Li, the 6Li/7Li abundance ratio observed in pre-main sequence (PMS) stars is ~ 0.5. The 6Li(p,a)3He and 6Li(p,g)7Be reactions are the main processes that contribute to 6Li destruction...
Dr
Umberto Battino
(University of Edinburgh)
04/09/2018, 15:07
The production of the proton-rich stable isotopes beyond iron that we observe today in the solar system is still uncertain. Core collapse supernovae (ccSNe) and thermonuclear supernovae (SNe Ia) exploding within the single-degenerate scenario have been proposed to be a potential source for these isotopes. Recent works performing Galactic Chemical Evolution (GCE) calculations, showed that...
Dr
Andreea Oprea
("Horia Hulubei” National Institute for Physics and Nuclear Engineering (IFIN-HH), Bucharest, Romania)
04/09/2018, 15:41
Preliminary alpha capture cross sections on Sr at energies close to the Gamow window will be presented. The cross sections were measured by means of the activation method using an alpha beam delivered by the Bucharest IFIN-HH 9MV tandem accelerator. The induced activities were measured with two large volume HPGe detectors in close geometry placed in a low background passive shielding. The...
Mr
Tibor Norbert Szegedi
(MTA Atomki)
04/09/2018, 15:58
Alpha-nucleus optical model potentials (OMP) are widely used in nuclear reaction network calculations aiming at the study of the gamma-process [1] and the weak r-process [2]. Considerable theoretical and experimental effort has been devoted in recent years to improve the knowledge of the OMP’s in order to give correct predictions for the cross sections and reaction rates [3,4] (and references...
David Jenkins Jenkins
(University of York)
06/09/2018, 14:00
The 12C+12C fusion reaction is one of the key reactions governing the evolution of massive stars as well as being critical to the physics underpinning various explosive astrophysical scenarios [1]. Our understanding of the 12C+12C reaction rate in the Gamow window – the energy range relevant to the different astrophysical scenarios – is presently confused. This is due to the large number of...
Dr
Sergio Cristallo
(INAF - Osservatorio Astronomico d'Abruzzo; INFN - Sezione di Perugia)
06/09/2018, 14:25
Nuclear astrophysics is an interdisciplinary field at the crossing of various branches, from experimental and theoretical studies of nuclear cross sections to stellar evolutionary models of high complexity. The physics of stellar interiors can be constrained only if the adopted inputs in stellar modelling are known with high accuracy. For the nucleosynthesis of heavy elements, neutron capture...
Dr
Matej Lipoglavsek
(Jozef Stefan Institute, Ljubljana, Slovenia)
06/09/2018, 14:43
We have studied the nuclear reaction d(p,gamma)He-3 in the proton energy range between 60 and 300 keV. This reaction is the second step of the primordial nucleosynthesis and our energies cover the range of energies after the Big-Bang. The reaction has previously not been studied very well in this energy range and the few existing cross section measurements do not agree with latest model...
Dr
Annamaria Mazzone
(BA)
06/09/2018, 15:19
Among the products of stellar nucleosynthesis heavier than Fe, 154Gd together with 152Gd have the peculiarity to be mainly produced by the slow capture process (the so-called s-process). Only a minor contribution may be produced in other processes. Their almost pure s-process origin makes them crucial for testing various models of the galactic chemical evolution (GCE). According to recent...
Alberto Mengoni
(BO),
Cristian Massimi
(BO)
06/09/2018, 15:37
Nuclear reactions responsible for the creation and destruction of Be-7 (the progenitor of Li-7), during Big Bang Nucleosynthesis (BBN), play the key role in the determination of the resulting primordial abundance of Li-7, the third chemical element formed during the very early phase of evolution of the Universe. Current standard BBN models predict a Li-7 abundance which is a factor of 2-3...
Stefan Reinicke
(Helmholtz-Zentrum Dresden-Rossendorf, Technische Universität Dresden)
06/09/2018, 15:55
The 12C(p,γ)13N reaction is relevant in several astrophysical scenarios, such as the early stages of the Bethe-Weizsäcker cycle of hydrogen burning and the production of 13C in stars on the asymptotic giant branch of the Hertzsprung-Russell diagram. Here new data on the 12C(p,γ)13N astrophysical S-factor at low energy, 0.1-0.5 MeV in the center of mass system are reported from an experiment in...
Silvia Traversi
(INFN Ferrara)
06/09/2018, 16:13
Binaries Neutron Stars (NSs) mergers can provide many constraints about
stellar composition because the evolution and features of these processes
strongly depends on the Equation Of State (EOS) of NSs. Indeed, the time
of the collapse after the merger, for given masses, is determined by the
softness of the EOS. Moreover, the process results in the ejection of
matter, both during the...
