Neutron star equation of state and GW170817

被引：11
|
作者：
Bhat, Sajad A. [1 ,2 ]
Bandyopadhyay, Debades [1 ,2 ]
机构：
[1] Saha Inst Nucl Phys, Astroparticle Phys & Cosmol Div, 1-AF Bidhannagar, Kolkata 700064, India
[2] Homi Bhabha Natl Inst, Training Sch Complex, Bombay 400094, Maharashtra, India
来源：
JOURNAL OF PHYSICS G-NUCLEAR AND PARTICLE PHYSICS | 2019年 / 46卷 / 01期
关键词：
neutron stars; dense matter; equations of state; gravitational waves;
D O I：
10.1088/1361-6471/aaef45
中图分类号：
O57 [原子核物理学、高能物理学];
学科分类号：
070202 ;
摘要：
Properties of neutron stars in GW170817 are investigated using different equations of state (EoS) involving nucleons, A hyperons, quarks resulting in 2 M-circle dot neutron stars. This calculation is performed using the same EoS for merger components and for low spin prior case. It is found from the computations of tidal deformability parameters that soft to moderately stiff EoS are allowed by the 50% and 90% credible regions obtained from the gravitational wave observation of binary neutron star merger GW170817, whereas the stiffest hadron-quark EoS which lies above the upper 90% limit, is ruled out. A correlation among the tidal deformabilities and masses is found to exist as already predicted. Furthermore moments of inertia and quadrupole moments of merger components of GW170817 are estimated.
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页数：11
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