VÖLKEL, Sebastian H., Roman KONOPLYA and Kostas D. KOKKOTAS. Inverse problem for Hawking radiation. Physical Review D. 2019, vol. 99, No 10, p. "104025-1"-"104025-9", 9 pp. ISSN 2470-0010. Available from: https://dx.doi.org/10.1103/PhysRevD.99.104025.
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Basic information
Original name Inverse problem for Hawking radiation
Authors VÖLKEL, Sebastian H. (276 Germany), Roman KONOPLYA (804 Ukraine, guarantor, belonging to the institution) and Kostas D. KOKKOTAS (300 Greece).
Edition Physical Review D, 2019, 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/47813059:19240/19:A0000432
Organization unit Faculty of Philosophy and Science in Opava
Doi http://dx.doi.org/10.1103/PhysRevD.99.104025
UT WoS 000467735900013
Keywords in English Hawking radiation; greybody factors; energy emission spectrum; black holes
Tags FÚ, GA19-03950S, RCTPA, RIVOK
Tags International impact, Reviewed
Links GA19-03950S, research and development project.
Changed by Changed by: Ing. Petra Skoumalová, učo 50554. Changed: 21/4/2020 10:32.
Abstract
In this work we study the inverse problem related to the emission of Hawking radiation. We first show how the knowledge of greybody factors of different angular contributions / can be used to constrain the width of the corresponding black hole perturbation potentials. Afterwards we provide a framework to recover the greybody factors from the actual energy emission spectrum, which has to be treated as the sum over all multipole numbers. The underlying method for the reconstruction of the potential widths is based on the inversion of the Gamow formula, a parabolic expansion and the Poschl-Teller potential. We define a "normalized" energy emission spectrum that turns out to be very beneficial for the numerical fitting process, as well as for an improved qualitative understanding of how much information of the black hole potentials are actually imprinted in the spectrum. The connection to recent studies on the inverse problem using the quasinormal spectra of ultracompact stars and exotic compact objects is discussed as well. In the Appendix we show that the spectrum can be approximated surprisingly well and simply with a parabolic expansion of the peak of the classical black hole scattering potentials.
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