A5100730161- Pulsars and Gravitational Waves Research
- High-Energy Particle Collisions Research
- Gamma-ray bursts and supernovae
- Particle physics theoretical and experimental studies
- Quantum Chromodynamics and Particle Interactions
- Geophysics and Gravity Measurements
- Shoulder Injury and Treatment
- High-pressure geophysics and materials
- Cosmology and Gravitation Theories
- Astrophysical Phenomena and Observations
- Scientific Research and Discoveries
Washington University in St. Louis
2021-2025
University of Houston
2023
Campbell Collaboration
2023
Abstract This review aims at providing an extensive discussion of modern constraints relevant for dense and hot strongly interacting matter. It includes theoretical first-principle results from lattice perturbative QCD, as well chiral effective field theory results. From the experimental side, it heavy-ion collision low-energy nuclear physics results, observations neutron stars their mergers. The validity different constraints, concerning specific conditions ranges applicability, is also provided.
Abstract In nuclear matter in isolated neutron stars, the flavor content (e.g., proton fraction) is subject to weak interactions, establishing ( β -)equilibrium. However, there can be deviations from this equilibrium during merger of two stars. We study resulting out-of-equilibrium dynamics collision by incorporating direct and modified Urca processes (in neutrino-transparent regime) into general-relativistic hydrodynamics simulations with a simplified neutrino transport scheme. demonstrate...
We analyze the isospin equilibration properties of neutrinoless nuclear ($npe$) matter in temperature and density range that is relevant to neutron star mergers. Our analysis incorporates neutrino-transparency corrections (``beta'') equilibrium condition which become noticeable at $T\ensuremath{\gtrsim}1\phantom{\rule{0.16em}{0ex}}\text{MeV}$. find relaxation rate rises rapidly as rises, $T\ensuremath{\approx}5\phantom{\rule{0.16em}{0ex}}\text{MeV}$ it comparable timescale oscillations occur...
We calculate the nonzero-temperature correction to beta equilibrium condition in nuclear matter under neutron star merger conditions, temperature range $1\,$MeV$ < T \lesssim 5\,$MeV. improve on previous work by using a consistent description of based IUF and SFHo relativistic mean field models. This includes dispersion relations for nucleons, which we show is essential these find that can be order $10$ $20\,$MeV, plays an important role correct calculation Urca rates, wrong factors or more...
This review aims at providing an extensive discussion of modern constraints relevant for dense and hot strongly interacting matter. It includes theoretical first-principle results from lattice perturbative QCD, as well chiral effective field theory results. From the experimental side, it heavy-ion collision low-energy nuclear physics results, observations neutron stars their mergers. The validity different constraints, concerning specific conditions ranges applicability, is also provided.
Exploring the equation of state dense matter is an essential part interpreting observable properties neutron stars. We present here first results for in zero-temperature limit generated by MUSES Calculation Engine, a composable workflow management system that orchestrates calculation and data processing stages comprising collection software modules designed within framework. The presented this work calculate equations using algorithms spanning three different theories/models: (1) Crust...
In nuclear matter in isolated neutron stars, the flavor content (e.g., proton fraction) is subject to weak interactions, establishing ($\beta$-)equilibrium. However, there can be deviations from this equilibrium during merger of two stars. We study resulting out-of-equilibrium dynamics collision by incorporating direct and modified Urca processes (in neutrino-transparent regime) into general-relativistic hydrodynamics simulations with a simplified neutrino transport scheme. demonstrate how...
Flavor-changing charged current (``Urca'') processes are of central importance in the astrophysics neutron stars. The standard approach is to approximate Urca rate as sum two contributions, direct and modified Urca. Attempts make calculations more accurate have been blocked by an unphysical divergence mUrca at dUrca threshold density. We argue that progress traditional separation into ``direct'' ``modified'' contributions should be replaced a single calculation consistently includes...
Flavor-changing charged current ("Urca") processes are of central importance in the astrophysics neutron stars. Standard calculations approximate Urca rate as sum two contributions, direct and modified Urca. Attempts to make more accurate have been impeded by an unphysical divergence at threshold density. In this paper we describe a systematically improvable approach where, simplest approximation, instead include imaginary part nucleon mass (nucleon width). The total is then obtained via...
We analyze the isospin equilibration properties of neutrino-transparent nuclear ($npe$) matter in temperature and density range that is relevant to neutron star mergers. Our analysis incorporates neutrino-transparency corrections (``beta'') equilibrium condition which become noticeable at $T\gtrsim 1\,$MeV. find relaxation rate rises rapidly as rises, $T\approx 5\,$MeV it comparable timescale oscillations occur immediately after merger. This produces a resonant peak bulk viscosity $T\sim...