Inferring the iron K emissivity profiles of accretion discs irradiated by extended coronae

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F24%3A00597511" target="_blank" >RIV/67985815:_____/24:00597511 - isvavai.cz</a>

Výsledek na webu

<a href="https://hdl.handle.net/11104/0355449" target="_blank" >https://hdl.handle.net/11104/0355449</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1093/mnras/stae1714" target="_blank" >10.1093/mnras/stae1714</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Inferring the iron K emissivity profiles of accretion discs irradiated by extended coronae

Popis výsledku v původním jazyce

One of the most promising methods to measure the spin of an accreting black hole is fitting the broad iron K alpha line in the X-ray spectrum. The line profile also depends on the geometry of the hard X-ray emitting corona. To put constraints on the black hole spin and corona geometry, it is essential to understand how do they affect the iron K alpha line emissivity profile. In this work, we present calculations of the illumination and the iron K alpha emissivity profiles performed with the Monte Carlo GR radiative transfer code monk. We focus on distinction between the illumination and emissivity profiles, which is in most previous studies neglected. We show that especially for the case of black hole X-ray binaries (BHXRBs), the difference is very large. For active galactic nuclei (AGNs), the emissivity profile has a more similar shape as the illumination profile, but it is notably steeper in the innermost region within a few gravitational radii. We find out that the different behaviour between AGN and BHXRB discs is due to the different energy spectra of the illuminating radiation. This suggests that the emissivity profile of the iron K alpha line cannot be determined by black hole spin and corona geometry alone and the energy spectrum of the illuminating radiation has to be taken into account. We also examined the effect of including the self-irradiation, and find it to be more important than the corona emission in BHXRBs.

Název v anglickém jazyce

Inferring the iron K emissivity profiles of accretion discs irradiated by extended coronae

Popis výsledku anglicky

One of the most promising methods to measure the spin of an accreting black hole is fitting the broad iron K alpha line in the X-ray spectrum. The line profile also depends on the geometry of the hard X-ray emitting corona. To put constraints on the black hole spin and corona geometry, it is essential to understand how do they affect the iron K alpha line emissivity profile. In this work, we present calculations of the illumination and the iron K alpha emissivity profiles performed with the Monte Carlo GR radiative transfer code monk. We focus on distinction between the illumination and emissivity profiles, which is in most previous studies neglected. We show that especially for the case of black hole X-ray binaries (BHXRBs), the difference is very large. For active galactic nuclei (AGNs), the emissivity profile has a more similar shape as the illumination profile, but it is notably steeper in the innermost region within a few gravitational radii. We find out that the different behaviour between AGN and BHXRB discs is due to the different energy spectra of the illuminating radiation. This suggests that the emissivity profile of the iron K alpha line cannot be determined by black hole spin and corona geometry alone and the energy spectrum of the illuminating radiation has to be taken into account. We also examined the effect of including the self-irradiation, and find it to be more important than the corona emission in BHXRBs.

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/GX21-06825X" target="_blank" >GX21-06825X: Akreující černé díry v nové éře polarizačních rentgenových misí</a><br>

Návaznosti

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Rok uplatnění

2024

Kód důvěrnosti údajů

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

Název periodika

Monthly Notices of the Royal Astronomical Society

ISSN

0035-8711

e-ISSN

1365-2966

Svazek periodika

532

Číslo periodika v rámci svazku

4

Stát vydavatele periodika

US - Spojené státy americké

Počet stran výsledku

11

Strana od-do

3786-3796

Kód UT WoS článku

001281876300011

EID výsledku v databázi Scopus

2-s2.0-85199917030