Dr
Ingo Tews
(INT Seattle)
08/02/2017, 09:00
Invited talk
Talk [Main Conference]
The neutron-matter equation of state connects several astrophysical systems over a wide density range. Among these are neutron-rich nuclei, which are relevant for the r-process, and neutron stars, which contain the densest form of matter we know to exist in the cosmos.
An accurate description of the neutron-matter equation of state is crucial to describe these systems and requires precise...
Dr
William Newton
(Texas A&M University-Commerce)
08/02/2017, 09:30
Contributed talk
Talk [Main Conference]
Nuclear pasta is a series of phases of complex nuclear matter arranged in a number of different geometries and topologies. We present 3D quantum calculations of nuclear pasta in neutron star crusts and proto-neutron stars. We find that, when quantum effects are included, nuclear pasta occurs at lower densities than predicted in semi-classical or classical models, and we predict that over 50%...
Prof.
hesham mansour
(Physics department,faculty of science,Cairo university,Egypt)
08/02/2017, 09:45
Contributed talk
Talk [Main Conference]
Static properties of nuclear matter e.g., binding energy, symmetry energy, etc.; can be determined by the (EOS), the (EOS) of nuclear matter has been of great interest in nuclear physics and astrophysics. The interest in the equation of state (EOS) of nuclear matter stems from different motivations and prospects. First, it appears as a theoretical challenge to the possibility of predicting,...
Andre da Silva Schneider
(California Institute of Technology)
08/02/2017, 10:00
Contributed talk
Talk [Main Conference]
The equation of state (EOS) of dense matter is an essential ingredient for numerical simulations of many astrophysical phenomena. We implement a modular open-source Fortran 90 code to construct the EOS of hot dense matter for astrophysical applications. For high density matter we use a non-relativistic liquid-drop description of nuclei that includes surface effects in a single nucleus...
Dr
Giordano Cerizza
(National Superconducting Cyclotron Laboratory (NSCL))
08/02/2017, 10:15
Contributed talk
Talk [Main Conference]
The nuclear equation of state is a fundamental property of nuclear matter that describes relationships between energy, pressure, temperature, density, and isospin asymmetry in a nuclear system. The asymmetric part of EoS, which is originated by the isospin asymmetry, has not been well constrained yet above the saturation density, contrary to the symmetric part of EoS. Transport model...