Inverse problem for Hawking radiation

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F47813059%3A19240%2F19%3AA0000432" target="_blank" >RIV/47813059:19240/19:A0000432 - isvavai.cz</a>

Výsledek na webu

<a href="https://journals.aps.org/prd/abstract/10.1103/PhysRevD.99.104025" target="_blank" >https://journals.aps.org/prd/abstract/10.1103/PhysRevD.99.104025</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1103/PhysRevD.99.104025" target="_blank" >10.1103/PhysRevD.99.104025</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Inverse problem for Hawking radiation

Popis výsledku v původním jazyce

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.

Název v anglickém jazyce

Inverse problem for Hawking radiation

Popis výsledku anglicky

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.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

<a href="/cs/project/GA19-03950S" target="_blank" >GA19-03950S: Testování silné gravitace prostřednictvím černých děr</a><br>

Návaznosti

P - Projekt vyzkumu a vyvoje financovany z verejnych zdroju (s odkazem do CEP)<br>I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Rok uplatnění

2019

Kód důvěrnosti údajů

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Název periodika

Physical Review D

ISSN

2470-0010

e-ISSN

2470-0029

Svazek periodika

99

Číslo periodika v rámci svazku

10

Stát vydavatele periodika

US - Spojené státy americké

Počet stran výsledku

9

Strana od-do

„104025-1“-„104025-9“

Kód UT WoS článku

000467735900013

EID výsledku v databázi Scopus

2-s2.0-85066426943