KONOPLYA, Roman. Further clarification on quasinormal modes/circular null geodesics correspondence. Physics Letters B. 2023, vol. 838, March 2023, p. "137674-1"-"137674-2", 4 pp. ISSN 0370-2693. Available from: https://dx.doi.org/10.1016/j.physletb.2023.137674.
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Basic information
Original name Further clarification on quasinormal modes/circular null geodesics correspondence
Authors KONOPLYA, Roman (804 Ukraine, guarantor, belonging to the institution).
Edition Physics Letters B, 2023, 0370-2693.
Other information
Original language English
Type of outcome Article in a journal
Field of Study 10308 Astronomy
Country of publisher Netherlands
Confidentiality degree is not subject to a state or trade secret
WWW URL
RIV identification code RIV/47813059:19630/23:A0000257
Organization unit Institute of physics in Opava
Doi http://dx.doi.org/10.1016/j.physletb.2023.137674
UT WoS 000972869200001
Keywords in English hole normal-modes;black-hole;WBK approach;instability; shadow
Tags RIV24, UF
Tags International impact, Reviewed
Links GA19-03950S, research and development project.
Changed by Changed by: Mgr. Pavlína Jalůvková, učo 25213. Changed: 12/2/2024 13:56.
Abstract
The well-known correspondence between quasinormal modes of any stationary, spherically symmetric and asymptotically flat or de Sitter black hole and parameters of the circular null geodesic was initially claimed for gravitational and test field perturbations. According to this correspondence the real and imaginary parts of the Z >> n quasinormal mode (where Z and n are multipole and overtone numbers respectively) are multiples of the frequency and instability timescale of the circular null geodesics respectively. Later it was shown that the correspondence is guaranteed only for test fields and may be broken for gravitational and other non-minimally coupled fields. Here, we further specify the correspondence and prove that even when it is guaranteed, it may not represent the full spectrum of the Z >> n modes, missing the quasinormal frequencies which cannot be found by the standard WKB method. In particular we show that this always happens for an arbitrary asymptotically de Sitter black holes and further argue that, in general, this might be related to sensitivity of the quasinormal spectrum to geometry deformations near the boundaries.
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