A New Constraint on the Nuclear Equation of State from Statistical Distributions of Compact Remnants of Supernovae

@article{Meskhi2021ANC,
  title={A New Constraint on the Nuclear Equation of State from Statistical Distributions of Compact Remnants of Supernovae},
  author={Mikhail M. Meskhi and Noah Wolfe and Zhenyu Dai and Carla Frohlich and Jonah Maxwell Miller and Raymond K. W. Wong and Ricardo Vilalta},
  journal={The Astrophysical Journal Letters},
  year={2021},
  volume={932}
}
Understanding how matter behaves at the highest densities and temperatures is a major open problem in both nuclear physics and relativistic astrophysics. Our understanding of such behavior is often encapsulated in the so-called high-temperature nuclear equation of state (EOS), which influences compact binary mergers, core-collapse supernovae, and other phenomena. Our focus is on the type (either black hole or neutron star) and mass of the remnant of the core collapse of a massive star. For each… 

References

SHOWING 1-10 OF 41 REFERENCES

Nuclear Equation of state for Compact Stars and Supernovae

The equation of state (EoS) of hot and dense matter is a fundamental input to describe static and dynamical properties of neutron stars, core-collapse supernovae and binary compact-star mergers. We

PUSHing Core-collapse Supernovae to Explosions in Spherical Symmetry. II. Explodability and Remnant Properties

In a previously presented proof-of-principle study, we established a parameterized spherically symmetric explosion method (PUSH) that can reproduce many features of core-collapse supernovae. The

Mass Ejection in Failed Supernovae: Equation of State and Neutrino Loss Dependence

A failed core-collapse supernova from a nonrotating progenitor can eject mass due to a weakening of gravity associated with neutrino emission from the protoneutron star. This mechanism yields

NEW HYPERON EQUATIONS OF STATE FOR SUPERNOVAE AND NEUTRON STARS IN DENSITY-DEPENDENT HADRON FIELD THEORY

We develop new hyperon equation of state (EoS) tables for core-collapse supernova simulations and neutron stars. These EoS tables are based on a density-dependent relativistic hadron field theory

Constraining the Maximum Mass of Neutron Stars from Multi-messenger Observations of GW170817

We combine electromagnetic (EM) and gravitational-wave (GW) information on the binary neutron star (NS) merger GW170817 in order to constrain the radii and maximum mass of NSs. GW170817 was followed

PSR J0030+0451 Mass and Radius from NICER Data and Implications for the Properties of Neutron Star Matter

Neutron stars are not only of astrophysical interest, but are also of great interest to nuclear physicists because their attributes can be used to determine the properties of the dense matter in

PUSHing Core-collapse Supernovae to Explosions in Spherical Symmetry. IV. Explodability, Remnant Properties, and Nucleosynthesis Yields of Low-metallicity Stars

In this fourth paper of the series, we use the parameterized, spherically symmetric explosion method PUSH to perform a systematic study of two sets of nonrotating stellar progenitor models. Our study

Modeling Kilonova Light Curves: Dependence on Nuclear Inputs

The mergers of binary neutron stars, as well as black hole–neutron star systems, are expected to produce an electromagnetic counterpart that can be analyzed to infer the element synthesis that

Core-collapse Supernovae: From Neutrino-driven 1D Explosions to Light Curves and Spectra

We present bolometric and broadband light curves and spectra for a suite of core-collapse supernova models exploded self-consistently in spherical symmetry within the PUSH framework. We analyze broad