KONOPLYA, Roman and A. ZHIDENKO. Nonoscillatory gravitational quasinormal modes and telling tails for Schwarzschild-de Sitter black holes. Physical Review D. 2022, vol. 106, No 12, p. "124004-1"-"124004-8", 8 pp. ISSN 2470-0010. Available from: https://dx.doi.org/10.1103/PhysRevD.106.124004.
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Basic information
Original name Nonoscillatory gravitational quasinormal modes and telling tails for Schwarzschild-de Sitter black holes
Authors KONOPLYA, Roman (804 Ukraine, belonging to the institution) and A. ZHIDENKO.
Edition Physical Review D, 2022, 2470-0010.
Other information
Original language English
Type of outcome Article in a journal
Field of Study 10308 Astronomy
Country of publisher United States of America
Confidentiality degree is not subject to a state or trade secret
WWW URL
RIV identification code RIV/47813059:19630/22:A0000192
Organization unit Institute of physics in Opava
Doi http://dx.doi.org/10.1103/PhysRevD.106.124004
UT WoS 000909780200003
Keywords in English quasinormal spectrum;gravitational perturbations;Schwarzschild-de Sitter black holes;oscillatory modes
Tags FÚ, RIV23
Tags International impact, Reviewed
Links GA19-03950S, research and development project.
Changed by Changed by: Mgr. Pavlína Jalůvková, učo 25213. Changed: 7/2/2023 08:55.
Abstract
We show that the quasinormal spectrum of gravitational perturbations of Schwarzschild-de Sitter black holes contains a new branch of purely imaginary modes. These modes are not algebraically special and we showed that the sum of them form the well-known in the literature exponential asymptotic tail. When the ratio of the event horizon radius to the cosmological horizon vanishes, these quasinormal modes approach modes of empty de Sitter spacetime. Thus, the spectrum consists of the two branches: Schwarzschild branch deformed by the cosmological constant and de Sitter branch deformed by the black hole mass. While the de Sitter branch contains purely imaginary modes only, the oscillatory modes (with nonzero real part) of the Schwarzschild branch can also become purely imaginary for some values of the cosmological constant, for which they approach the algebraically special mode.
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