Nuclear Theory·nucl-th

Wednesday·October 5, 2016

10 papers—7 primary·3 cross-listed

08
Probing the nature of phases across the phase transition at finite isospin chemical potential
Gunnar S. Bali🇩🇪 · G. Endrodi🇩🇪 · Rajiv V. Gavai🇮🇳 · N. Mathur🇮🇳
We compare the low eigenvalue spectra of the Overlap Dirac operator on two sets of configurations at $μ_{I} / μ_{I}^{c}$ = 0.5 and 1.5 generated with dynamical staggered fermions at these isospin chemical potential on $2 4^{3} \times 6$ lattices. We find very small changes in the number of zero modes and low lying modes which is in stark contrast with those across the corresponding finite temperature phases where one sees a drop across the phase transition. Possible consequences are discussed.
↳ hep-lathep-phnucl-thActa Phys.Polon.Supp.(2017)·6 citations
09
A fast algorithm for radiative transport in isotropic media
Kui Ren · Rongting Zhang · Yimin Zhong
We propose in this work a fast numerical algorithm for solving the equation of radiative transfer (ERT) in isotropic media. The algorithm has two steps. In the first step, we derive an integral equation for the angularly averaged ERT solution by taking advantage of the isotropy of the scattering kernel, and solve the integral equation with a fast multipole method (FMM). In the second step, we solve a scattering-free transport equation to recover the original ERT solution. Numerical simulations are presented to demonstrate the performance of the algorithm for both homogeneous and inhomogeneous media.
↳ math.NAcs.NAnucl-thphysics.comp-phJ.Comput.Phys.(2019)·0 citations
10
Equation of State for Nucleonic and Hyperonic Neutron Stars with Mass and Radius Constraints
Laura Tolos🇪🇸 · Mario Centelles🇪🇸 · Angels Ramos🇪🇸
We obtain a new equation of state for the nucleonic and hyperonic inner core of neutron stars that fulfills the 2 $M_{⊙}$ observations as well as the recent determinations of stellar radii below 13 km. The nucleonic equation of state is obtained from a new parametrization of the FSU2 relativistic mean-field functional that satisfies these latest astrophysical constraints and, at the same time, reproduces the properties of nuclear matter and finite nuclei while fulfilling the restrictions on high-density matter deduced from heavy-ion collisions. On the one hand, the equation of state of neutron star matter is softened around saturation density, which increases the compactness of canonical neutron stars leading to stellar radii below 13 km. On the other hand, the equation of state is stiff enough at higher densities to fulfill the 2 $M_{⊙}$ limit. By a slight modification of the parametrization, we also find that the constraints of 2 $M_{⊙}$ neutron stars with radii around 13 km are satisfied when hyperons are considered. The inclusion of the high magnetic fields present in magnetars further stiffens the equation of state. Hyperonic magnetars with magnetic fields in the surface of $\sim 1 0^{15}$ G and with values of $\sim 1 0^{18}$ G in the interior can reach maximum masses of 2 $M_{⊙}$ with radii in the 12-13 km range.
↳ astro-ph.HEastro-ph.SRnucl-thApJ(2017)·135 citations

Affiliations

first authorsco-authorsvia INSPIRE

Probing the nature of phases across the phase transition at finite isospin chemical potential

A fast algorithm for radiative transport in isotropic media

Equation of State for Nucleonic and Hyperonic Neutron Stars with Mass and Radius Constraints

Affiliations