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Nuclear Physics in Astrophysics VIII

18–23 Jun 2017
Laboratori Nazionali del Sud
Europe/Rome timezone

Session

r-process 3

20 Jun 2017, 17:10
Sala conferenze (Laboratori Nazionali del Sud)

Sala conferenze

Laboratori Nazionali del Sud

Via S. Sofia 62 I-95123 Catania Italy

Presentation materials

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  1. 130. Nuclear masses and the r-process astrophysical site
    Prof. Rebecca Surman (University of Notre Dame)
    20/06/2017, 17:10
    Invited talk
    The key role played by nuclear masses in rapid neutron capture, or r-process, nucleosynthesis has long been recognized. Masses set the reaction flow path for an r-process in equilibrium and influence the neutron capture rates, beta decay rates, and fission properties that determine the final abundances. Here we describe modern efforts to quantify the uncertainties in r-process abundance...
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  2. 48. Beta-delayed neutron emission probability measurements for r process studies at RIKEN RIBF
    Gabor Kiss (RIKEN Nishina Center)
    20/06/2017, 17:40
    Explosive scenarios in astrophysics: observations, theory, and experiments
    Invited talk
    About 50% of the isotopes heavier than iron are synthesized in the so-called astrophysical r-process [1]. During the explosion of a type II supernovae or a Neutron star merger exotic isotopes, closed to the drip line are formed via rapid neutron capture reactions [2]. These, very neutron-rich nuclei emit neutrons after the beta-decay when the decay Q-value is larger than the neutron separation...
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  3. 87. Neutron capture rates for the astrophysical r process
    Artemis Spyrou (NSCL/MSU)
    20/06/2017, 18:10
    Explosive scenarios in astrophysics: observations, theory, and experiments
    Oral
    % % 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 ...
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  4. 70. Equation of State and in-medium nuclear structure in heavy-ion collisions
    Giuseppe Verde (CT)
    20/06/2017, 18:30
    Neutron stars and the equation of state of dense matter
    Oral
    Heavy-ion collisions provide unique access to nuclear structure properties away from saturation density and at finite temperatures. Such structure properties are determined by the equation of state (EoS) and the symmetry energy of nuclear matter that can in turn be studied under laboratory controlled conditions. Such conditions are encountered in neutron stars and in core collapse supernovae...
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  5. 38. Constraining The Symmetry Energy (Far) Above Saturation Density Using Elliptic Flow
    Dr Dan Cozma (IFIN-HH)
    20/06/2017, 18:50
    Neutron stars and the equation of state of dense matter
    Oral
    Using a quantum molecular dynamics type transport model coupled to a phase-space coalescence algorithm to determine final spectra of intermediate energy heavy-ion collisions it has been shown that the elliptic flow ratios of neutrons-to-protons and neutrons-to-hydrogen probe, on average, different density regimes of the compressed nuclear matter created in such reactions [1]. This fact is used...
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