QNP2022 - The 9th International Conference on Quarks and Nuclear Physics

Session

Neutron Stars & EoS

Sep 6, 2022, 12:30 PM

online

Conveners

Neutron Stars & EoS: Parallel 3

• Jocelyn Read (CSU Fullerton)

Neutron Stars & EoS: Parallel 3

• Jorge Piekarewicz (Florida State University)

114. From hadrons to quarks in neutron stars

TORU KOJO (Tohoku University)

9/6/22, 12:30 PM

I discuss neutron star matter from the picture of quark-hadron continuity. Recent neutron observations indicate that 2.1- and 1.4-solar mass neutron stars have similar radii, disfavoring the presence of strong first order phase transitions in the domain between ~2n0 and ~5n0 with n0 being nuclear saturation density. Meanwhile ~5n0 is the density where baryons are expected to overlap and...

119. From outer space to deep inside: exploring neutron skins

Michaela Thiel

9/6/22, 12:55 PM

The Equation of State (EoS) links together fundamental properties of nuclear matter. Heavy nuclei, though orders of magnitude smaller than neutron stars, are governed by the same underlying physics, which is enshrined in the EoS. An accurate and model-independent determination of the neutron-skin thickness of heavy nuclei, using parity-violating electron scattering, provides significant...

163. The PREX and CREX neutron density experiments and neutron stars

Charles Horowitz

9/6/22, 1:20 PM

The PREX and CREX experiments at Jefferson Laboratory use parity violating electron scattering to cleanly locate neutrons in neutron rich nuclei. These measurements demonstrate that heavy nuclei have a neutron rich skin and measure its thickness. This determines the pressure of neutron rich matter and has important implications for the structure of neutron stars. We compare PREX results in...

14. Exploring Neutron stars EoS with coherent π0 π0 photoproduction at A2@MAMI

Mihai Mocanu (University of York / JLab)

9/6/22, 1:45 PM

Recent measurement of coherent π0 photoproduction on Pb lead to a most accurate determination of the neutron skin, constraining nuclear matter Equation of State (EoS) at around ρ~1ρ0. A natural next step is elucidating the nuclear EoS at higher densities to tune our understanding of the most violent process in the Universe - neutron stars mergers. It was demonstrated that at densities above...

245. Neutron stars in gravitational-wave astronomy

Jocelyn Read (CSU Fullerton)

9/6/22, 3:00 PM

oral presentation

The gravitational-wave observatories of LIGO and Virgo have opened a new field of astronomy. The first and nearest signal from merging neutron stars, GW170817, guided astronomical partners' observations, constrained the source system's properties, and gave a new viewpoint on the equation of state of dense matter in neutron stars. More distant sources primarily tell us about the source masses,...

164. Hot and cold neutron stars in the Quark-Meson-Coupling model

Dr Jirina Stone (University of Oxford/University of Tennessee)

9/6/22, 3:25 PM

In the relativistic mean-field Quark-Meson-Coupling (QMC) model, the baryon-baryon interaction in medium is interpreted in terms of a virtual meson exchange between light valence quarks in individual baryons [1]. This unique feature leads to a dramatic reduction of variable parameters of the model as compared to traditional nuclear structure models, and to a versatile application to high...

106. Sound velocity beyond the High-Density Relativistic Limit from Lattice Simulation of Dense Two-Color QCD

Etsuko Itou (iTHEMS, RIKEN)

9/6/22, 3:50 PM

We obtain the equation of state (EoS) for two-color QCD at low temperature and high density from the lattice Monte Carlo simulation. We find that the velocity of sound exceeds the relativistic limit (cs2/c2=1/3) after BEC-BCS crossover in the superfluid phase. Such an excess of the sound velocity is predicted by several effective theories but is previously unknown from any lattice calculations...

3. Model independent constraints on dense matter equation of state

NARESH KUMAR PATRA (BITS Pilani K K Birla Goa Campus, NH-B, South Goa, Goa, Pin-757040)

9/6/22, 4:15 PM

We construct posterior distributions of equations of state (EoS),
relevant to the studies of neutron stars (NSs), by applying Bayesian
approach to two different models. The EoSs are subjected to minimal
constraints which correspond to a few basic properties of nuclear
matter at the saturation density and the low density pure neutron
matter EoS obtained from a precise...

190. Quantum Monte Carlo studies of nuclear systems

Dr Maria Piarulli (Washington University )

A major goal of nuclear theory is to explain the wealth of data and peculiarities exhibited by nuclear systems using a fully microscopic approach. In this approach, which we refer to as the basic model of nuclear theory, nucleons interact with each other via many-body (primarily two- and three-body) effective interactions, and with external electroweak probes via effective currents describing...