Quasinormal modes as a distinguisher between general relativity and f (R) gravity

被引：38

作者：

Bhattacharyya, Soham ^{[1
]}

Shankaranarayanan, S. ^{[1
,2
]}

机构：

[1] Indian Inst Sci Educ & Res Thiruvananthapuram IIS, Sch Phys, Trivandrum 695016, Kerala, India

[2] Indian Inst Technol, Dept Phys, Bombay 400076, Maharashtra, India

来源：

PHYSICAL REVIEW D | 2017年 / 96卷 / 06期

关键词：

BLACK-HOLES; GRAVITATIONAL-RADIATION; PERTURBATIONS; SCATTERING; WAVES;

D O I：

10.1103/PhysRevD.96.064044

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Quasinormal modes (QNMs) or the ringdown phase of gravitational waves provide critical information about the structure of compact objects like black holes. Thus, QNMs can be a tool to test general relativity (GR) and possible deviations from it. In the case of GR, it has been known for a long time that a relation between two types of black hole perturbations-scalar (Zerilli) and vector (Regge-Wheeler)-leads to an equal share of emitted gravitational energy. With the direct detection of gravitational waves, it is now natural to ask whether the same relation (between scalar and vector perturbations) holds for modified gravity theories, and if not, whether one can use this as a way to probe deviations from general relativity. As a first step, we show explicitly that the above relation between Regge-Wheeler and Zerilli perturbations breaks down for a general f(R) model and hence the two perturbations do not share equal amounts of emitted gravitational energy. We discuss the implication of this imbalance for observations and the no-hair conjecture.

引用

页数：10

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