Minimum X-ray source size of the on-axis corona in AGN

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F16%3A00463892" target="_blank" >RIV/67985815:_____/16:00463892 - isvavai.cz</a>

Výsledek na webu

<a href="http://dx.doi.org/10.1002/asna.201612327" target="_blank" >http://dx.doi.org/10.1002/asna.201612327</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1002/asna.201612327" target="_blank" >10.1002/asna.201612327</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Minimum X-ray source size of the on-axis corona in AGN

Popis výsledku v původním jazyce

The "lamppost" model is often used to describe the X-ray source geometry in AGN, where an infinitesimal point source is located on the black hole spin axis. This is especially invoked for narrow line Seyfert 1 (NLS1) galaxies, where an extremely broad iron line seen in episodes of low X-ray flux can both be explained by extremely strong relativistic effects as the source approaches the black hole horizon. The most extreme spectrum seen from the NLS1 1H0707-495 requires that the source is less than 1GM/c(2) above the event horizon in this geometry. However, the source must also be large enough to intercept sufficient seed photons from the disc to make the hard X-ray Compton continuum which produces the observed iron line/reflected spectrum. We use a fully relativistic ray tracing code to show that this implies that the source must be substantially larger than 1GM/c(2) in 1H0707-495 if the disc is the source of seed photons. Hence the source cannot fit as close as 1GM/c(2) to the horizon, so the observed spectrum and variability are not formed purely by effects of strong gravity but probably also by changes in corona and inner accretion flow geometry

Název v anglickém jazyce

Minimum X-ray source size of the on-axis corona in AGN

Popis výsledku anglicky

The "lamppost" model is often used to describe the X-ray source geometry in AGN, where an infinitesimal point source is located on the black hole spin axis. This is especially invoked for narrow line Seyfert 1 (NLS1) galaxies, where an extremely broad iron line seen in episodes of low X-ray flux can both be explained by extremely strong relativistic effects as the source approaches the black hole horizon. The most extreme spectrum seen from the NLS1 1H0707-495 requires that the source is less than 1GM/c(2) above the event horizon in this geometry. However, the source must also be large enough to intercept sufficient seed photons from the disc to make the hard X-ray Compton continuum which produces the observed iron line/reflected spectrum. We use a fully relativistic ray tracing code to show that this implies that the source must be substantially larger than 1GM/c(2) in 1H0707-495 if the disc is the source of seed photons. Hence the source cannot fit as close as 1GM/c(2) to the horizon, so the observed spectrum and variability are not formed purely by effects of strong gravity but probably also by changes in corona and inner accretion flow geometry

Druh

J_x - Nezařazeno - Článek v odborném periodiku (Jimp, Jsc a Jost)

CEP obor

BN - Astronomie a nebeská mechanika, astrofyzika

OECD FORD obor

—

Projekt

—

Návaznosti

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Rok uplatnění

2016

Kód důvěrnosti údajů

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

Název periodika

Astronomische Nachrichten

ISSN

0004-6337

e-ISSN

—

Svazek periodika

337

Číslo periodika v rámci svazku

4-5

Stát vydavatele periodika

DE - Spolková republika Německo

Počet stran výsledku

7

Strana od-do

441-447

Kód UT WoS článku

000375725600017

EID výsledku v databázi Scopus

2-s2.0-84964793148