A matrix method for quasinormal modes: Kerr and Kerr-Sen black holes

被引：36

作者：

Lin, Kai ^{[1
,2
,3
]}

Qian, Wei-Liang ^{[3
,4
]}

Pavan, Alan B. ^{[1
]}

Abdalla, Elcio ^{[5
]}

机构：

[1] Univ Fed Itajuba, Inst Fis, Itajuba, MG, Brazil

[2] China West Normal Univ, Dept Astron, Nanchong 637002, Sichuan, Peoples R China

[3] Univ Sao Paulo, Escola Engn Lorena, Lorena, SP, Brazil

[4] Univ Estadual Paulista, Fac Engn Guaratingueta, Guaratingueta, SP, Brazil

[5] Univ Sao Paulo, Inst Fis, Sao Paulo, Brazil

来源：

MODERN PHYSICS LETTERS A | 2017年 / 32卷 / 25期

基金：

巴西圣保罗研究基金会; 中国国家自然科学基金;

关键词：

Kerr black hole; Kerr-Sen black hole; quasinormal modes; Taylor series; Teukolsky equation; LATE-TIME BEHAVIOR; STELLAR COLLAPSE; EXPLOSIONS; FIELD;

D O I：

10.1142/S0217732317501346

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

In this paper, a matrix method is employed to study the scalar quasinormal modes of Kerr as well as Kerr-Sen black holes. Discretization is applied to transfer the scalar perturbation equation into a matrix form eigenvalue problem, where the resulting radial and angular equations are derived by the method of separation of variables. The eigenvalues, quasinormal frequencies omega and angular quantum numbers lambda, are then obtained by numerically solving the resultant homogeneous matrix equation. This work shows that the present approach is an accurate, as well as efficient method for investigating quasinormal modes.

引用

页数：9

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