Axial quasinormal modes of neutron stars in R2 gravity

被引：17

作者：

Blazquez-Salcedo, Jose Luis ^{[1
]}

Doneva, Daniela D. ^{[2
,3
]}

Kunz, Jutta ^{[1
]}

Staykov, Kalin V. ^{[4
]}

Yazadjiev, Stoytcho S. ^{[2
,4
,5
]}

机构：

[1] Carl von Ossietzky Univ Oldenburg, Inst Phys, Postfach 2503, D-26111 Oldenburg, Germany

[2] Eberhard Karls Univ Tubingen, Theoret Astrophys, D-72076 Tubingen, Germany

[3] Bulgarian Acad Sci, INRNE, BU-1784 Sofia, Bulgaria

[4] Sofia Univ, Dept Theoret Phys, Fac Phys, Sofia 1164, Bulgaria

[5] Bulgarian Acad Sci, Inst Math & Informat, Acad G Bonchev St 8, BU-1113 Sofia, Bulgaria

来源：

PHYSICAL REVIEW D | 2018年 / 98卷 / 10期

关键词：

EQUATION-OF-STATE; GRAVITATIONAL-WAVES;

D O I：

10.1103/PhysRevD.98.104047

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

In the present paper, the axial quasinormal modes of neutron stars in f(R) gravity are examined using a large set of equations of state. The numerical calculations are made using two different approaches: performing time evolution of the perturbation equations and solving the time-independent representation of the equations as a boundary value problem. According to the results, the mode frequencies and the damping times decrease with the increase of the free parameter of the theory in comparison to the pure general relativistic case. While the frequencies deviate significantly from Einstein's theory for all realistic neutron star masses (say above 1 M-circle dot), the damping times reach non-negligible differences only for the more massive models. We have constructed as well universal (equation of state-independent) gravitational wave asteroseismology relations involving the frequencies and the damping times. It turns out that the equation-of-state independence is preserved using the same normalization as in pure general relativity. We discuss the differences of the phenomenological relations with respect to Einstein's theory of gravity for several values of the free parameter in f(R) gravity.

引用

页数：11

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