MICRA2019 - Microphysics In Computational Relativistic Astrophysics

Session

Equation of State

14 Aug 2019, 09:00

Abbeanum-Ground floor-HS1 - Hörsaal 1 (Jena FSU)

29. The Hadronic Equation of State for Neutron Stars

Dr Laura Tolos (Institute for Theoretical Physics, Goethe University )

14/08/2019, 09:00

Oral Contribution

The equation of state (EoS) of dense hadronic matter is of crucial importance for the description of the static and dynamical properties of neutron stars. In this talk I will review the current status of the hadronic EoS for neutron stars, from the point of both ab-initio many-body approaches and phenomenological models. The theoretical predictions for the hadronic EoS will be compared to the...

12. Equation of State Effects in the Core Collapse of Massive Stars

André da Silva Schneider (Stockholm University)

14/08/2019, 10:15

Oral Contribution

Uncertainties in our knowledge of the properties of dense matter near and above nuclear saturation density are among the main sources of variations in multi-messenger signatures predicted for the core collapse of massive stars and the properties of the resulting remnants. In this talk, I discuss how variations in the equation of state of dense matter affect the core collapse of massive stars....

15. Neutrino emission and equation of state in core collapse supernovae

Kosuke Sumiyoshi (National Institute of Technology, Numazu College)

14/08/2019, 11:00

Oral Contribution

I would like to report the recent progress on microphysics and supernova neutrinos utilizing our numerical simulations based on Boltzmann equation. As recent progress of core-collapse supernova simulations is rapid toward the first principle type calculations, remaining uncertainties of the microphysics are becoming important.

We have been developing the data table of equation of state...

6. Core-collapse supernovae and equation of state effects*

Hannah Yasin

14/08/2019, 11:30

Oral Contribution

Core-collapse supernovae (CCSN) are cosmic laboratories for physics at the extremes and numerical simulations are essential to help us understand the underlying mechanisms in these events. A key ingredient in simulations is the equation of state (EOS), which determines the contraction behavior of the proto-neutron star (PNS) and thus impacts neutrino energies and explosion dynamics. However,...

10. A unified quark-hadron equation of state

Niels-Uwe Bastian (University of Wroclaw)

14/08/2019, 14:00

Oral Contribution

The aim of our work is to develop a unified equation of state (EoS) for nuclear and quark matter for a wide range in temperature, baryon density and iso-spin asymmetry, which will make it applicable for heavy-ion collisions as well as for the astrophysics of neutron stars, neutron-star mergers and supernova explosions.
As a first step, we use improved EoS for the hadronic and quark matter...

5. Optimal neutron-star mass ranges to constrain the equation of state of nuclear matter with electromagnetic and gravitational-wave observations

Lukas Weih (Goethe University, Frankfurt)

14/08/2019, 14:30

Oral Contribution

Exploiting a very large library of physically plausible equations of state (EOSs) containing more than $10^7$ members and yielding more than $10^9$ stellar models, we conduct a survey of the impact that a neutron-star radius measurement via electromagnetic observations can have on the EOS of nuclear matter. Such measurements are soon to be expected from the ongoing NICER mission and will...