Radial oscillations of dark matter admixed neutron stars

被引：31

作者：

Routaray, Pinku ^{[1
]}

Das, H. C. ^{[2
,3
]}

Sen, Souhardya ^{[1
]}

Kumar, Bharat ^{[1
]}

Panotopoulos, Grigoris ^{[4
]}

Zhao, Tianqi ^{[5
]}

机构：

[1] Natl Inst Technol, Dept Phys & Astron, Rourkela 769008, India

[2] Inst Phys, Sachivalaya Marg, Bhubaneswar 751005, India

[3] Homi Bhabha Natl Inst, Training Sch Complex, Mumbai 400094, India

[4] Univ La Frontera, Dept Ciencias Fis, Casilla 54-D, Temuco 4811186, Chile

[5] Ohio Univ, Dept Phys & Astron, Athens, OH 45701 USA

来源：

PHYSICAL REVIEW D | 2023年 / 107卷 / 10期

关键词：

GRAVITATIONAL-WAVES; DENSE MATTER; PULSATIONS; EQUATION; MODES; GW170817; STATE;

D O I：

10.1103/PhysRevD.107.103039

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Within the relativistic mean-field model, we investigate the properties of dark matter (DM) admixed neutron stars, considering nonrotating objects made of isotropic matter. We adopt the IOPB-I hadronic equation of state (EOS) by assuming that the fermionic DM within supersymmetric models has already been accreted inside the neutron star (NS). The impact of DM on the mass-radius relationships and the radial oscillations of pulsating DM admixed neutron stars (with and without the crust) are explored. It is observed that the presence of DM softens the EOS, which in turn lowers the maximum mass and its corresponding radius. Moreover, adding DM results in higher frequencies of pulsating objects, and hence we show the linearity of the fundamental mode frequency of canonical NS with DM Fermi momentum. We also investigate the profile of eigenfunctions solving the Sturm-Liouville boundary value problem and verify its validity. Further, we study the stability of NSs considering the fundamental mode frequency variation with the mass of the star and verify the stability criterion partial differential M/ partial differential rho c > 0. Finally, the effect of the crust on the large frequency separation for different DM Fermi momenta is shown as well.

引用

页数：10

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