Properties of Neutron Stars with hyperon cores in parameterized hydrostatic conditions. (arXiv:1812.03529v1 [nucl-th])
<a href="http://arxiv.org/find/nucl-th/1/au:+Sen_D/0/1/0/all/0/1">Debashree Sen</a>, <a href="http://arxiv.org/find/nucl-th/1/au:+Banerjee_K/0/1/0/all/0/1">Kinjal Banerjee</a>, <a href="http://arxiv.org/find/nucl-th/1/au:+Jha_T/0/1/0/all/0/1">T.K. Jha</a>
Models of neutron stars (NSs) with hyperon cores are constructed with an
effective chiral model in mean-field approximation. The hyperon couplings are
fixed by reproducing their experimentally determined binding energies. The
impact of these couplings on population of different particles and the equation
of state (EoS) are studied in this work. The global properties of NSs like
gravitational mass, radius, baryonic mass and central density are calculated
using parameterized Tolman-Oppenheimer-Volkoff equations (PTOV) with special
emphasis on two effects of pressure – one contributing to total mass density
and the other to self gravity of the star. We find that with PTOV solutions in
static conditions, a softer EoS (including hyperons) can also lead to massive
stellar configurations of NSs, which are in well agreement with the observed
maximum mass bound of $approx 2 M_{odot}$ (PSR J0348-0432). Estimates of
$R_{1.4}$ and $R_{1.6}$, obtained with the PTOV equations are consistent with
the recent findings of the same from the data analysis of gravitational waves
(GW170817) observation.
Keywords: Neutron Star; Hyperons; Equation of State; parameterized
Tolman-Oppenheimer-Volkoff equations
Models of neutron stars (NSs) with hyperon cores are constructed with an
effective chiral model in mean-field approximation. The hyperon couplings are
fixed by reproducing their experimentally determined binding energies. The
impact of these couplings on population of different particles and the equation
of state (EoS) are studied in this work. The global properties of NSs like
gravitational mass, radius, baryonic mass and central density are calculated
using parameterized Tolman-Oppenheimer-Volkoff equations (PTOV) with special
emphasis on two effects of pressure – one contributing to total mass density
and the other to self gravity of the star. We find that with PTOV solutions in
static conditions, a softer EoS (including hyperons) can also lead to massive
stellar configurations of NSs, which are in well agreement with the observed
maximum mass bound of $approx 2 M_{odot}$ (PSR J0348-0432). Estimates of
$R_{1.4}$ and $R_{1.6}$, obtained with the PTOV equations are consistent with
the recent findings of the same from the data analysis of gravitational waves
(GW170817) observation.
Keywords: Neutron Star; Hyperons; Equation of State; parameterized
Tolman-Oppenheimer-Volkoff equations
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