Rotating neutron stars with quark cores. (arXiv:2102.04067v3 [nucl-th] UPDATED)
<a href="http://arxiv.org/find/nucl-th/1/au:+Rather_I/0/1/0/all/0/1">I. A. Rather</a>, <a href="http://arxiv.org/find/nucl-th/1/au:+Rahaman_U/0/1/0/all/0/1">Usuf Rahaman</a>, <a href="http://arxiv.org/find/nucl-th/1/au:+Imran_M/0/1/0/all/0/1">M. Imran</a>, <a href="http://arxiv.org/find/nucl-th/1/au:+Das_H/0/1/0/all/0/1">H. C. Das</a>, <a href="http://arxiv.org/find/nucl-th/1/au:+Usmani_A/0/1/0/all/0/1">A. A. Usmani</a>, <a href="http://arxiv.org/find/nucl-th/1/au:+Patra_S/0/1/0/all/0/1">S. K. Patra</a>
The rotating neutron star properties are studied with a phase transition to
quark matter. The density-dependent relativistic mean-field model (DD-RMF) is
employed to study the hadron matter, while the Vector-Enhanced Bag model (vBag)
model is used to study the quark matter. The star matter properties like mass,
radius,the moment of inertia, rotational frequency, Kerr parameter, and other
important quantities are studied to see the effect on quark matter. The maximum
mass of rotating neutron star with DD-LZ1 and DD-MEX parameter sets is found to
be around 3$M_{odot}$ for pure hadronic phase and decreases to a value around
2.6$M_{odot}$ with phase transition to quark matter, which satisfies the
recent GW190814 constraints. For DDV, DDVT, and DDVTD parameter sets, the
maximum mass decreases to satisfy the 2$M_{odot}$. The moment of inertia
calculated for various DD-RMF parameter sets decreases with the increasing mass
satisfying constraints from various measurements. Other important quantities
calculated also vary with the bag constant and hence show that the presence of
quarks inside neutron stars can also allow us to constraint these quantities to
determine a proper EoS. Also, the theoretical study along with the accurate
measurement of uniformly rotating neutron star properties may offer some
valuable information concerning the high-density part of the equation of state.
The rotating neutron star properties are studied with a phase transition to
quark matter. The density-dependent relativistic mean-field model (DD-RMF) is
employed to study the hadron matter, while the Vector-Enhanced Bag model (vBag)
model is used to study the quark matter. The star matter properties like mass,
radius,the moment of inertia, rotational frequency, Kerr parameter, and other
important quantities are studied to see the effect on quark matter. The maximum
mass of rotating neutron star with DD-LZ1 and DD-MEX parameter sets is found to
be around 3$M_{odot}$ for pure hadronic phase and decreases to a value around
2.6$M_{odot}$ with phase transition to quark matter, which satisfies the
recent GW190814 constraints. For DDV, DDVT, and DDVTD parameter sets, the
maximum mass decreases to satisfy the 2$M_{odot}$. The moment of inertia
calculated for various DD-RMF parameter sets decreases with the increasing mass
satisfying constraints from various measurements. Other important quantities
calculated also vary with the bag constant and hence show that the presence of
quarks inside neutron stars can also allow us to constraint these quantities to
determine a proper EoS. Also, the theoretical study along with the accurate
measurement of uniformly rotating neutron star properties may offer some
valuable information concerning the high-density part of the equation of state.
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