TWO-BODY RELAXATION DRIVEN EVOLUTION OF THE YOUNG STELLAR DISK IN THE GALACTIC CENTER

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F14%3A10287236" target="_blank" >RIV/00216208:11320/14:10287236 - isvavai.cz</a>

Výsledek na webu

<a href="http://dx.doi.org/10.1088/0004-637X/786/2/121" target="_blank" >http://dx.doi.org/10.1088/0004-637X/786/2/121</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1088/0004-637X/786/2/121" target="_blank" >10.1088/0004-637X/786/2/121</a>

Jazyk výsledku

angličtina

Název v původním jazyce

TWO-BODY RELAXATION DRIVEN EVOLUTION OF THE YOUNG STELLAR DISK IN THE GALACTIC CENTER

Popis výsledku v původním jazyce

The center of our Galaxy hosts almost two hundred very young stars, a subset of which is orbiting the central supermassive black hole (SMBH) in a relatively thin disk-like structure. First analyses indicated a power-law surface density profile of the disk, S. R-beta with beta = -2. Recently, however, doubts about this profile arose. In particular, it now seems to be better described by a sort of broken power law. By means of both analytical arguments and numerical N-body modeling, we show that such a broken power-law profile is a natural consequence of the two-body relaxation of the disk. Due to the small relative velocities of the nearby stars in co-planar Keplerian orbits around the SMBH, two-body relaxation is effective enough to affect the evolution of the disk on timescales comparable to its estimated age. In the inner, densest part of the disk, the profile becomes rather flat (beta approximate to - 1) while the outer parts keep imprints of the initial state. Our numerical models

Název v anglickém jazyce

TWO-BODY RELAXATION DRIVEN EVOLUTION OF THE YOUNG STELLAR DISK IN THE GALACTIC CENTER

Popis výsledku anglicky

The center of our Galaxy hosts almost two hundred very young stars, a subset of which is orbiting the central supermassive black hole (SMBH) in a relatively thin disk-like structure. First analyses indicated a power-law surface density profile of the disk, S. R-beta with beta = -2. Recently, however, doubts about this profile arose. In particular, it now seems to be better described by a sort of broken power law. By means of both analytical arguments and numerical N-body modeling, we show that such a broken power-law profile is a natural consequence of the two-body relaxation of the disk. Due to the small relative velocities of the nearby stars in co-planar Keplerian orbits around the SMBH, two-body relaxation is effective enough to affect the evolution of the disk on timescales comparable to its estimated age. In the inner, densest part of the disk, the profile becomes rather flat (beta approximate to - 1) while the outer parts keep imprints of the initial state. Our numerical models

Druh

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

CEP obor

BN - Astronomie a nebeská mechanika, astrofyzika

OECD FORD obor

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Projekt

<a href="/cs/project/LD12065" target="_blank" >LD12065: Černé díry a jejich okolí</a><br>

Návaznosti

P - Projekt vyzkumu a vyvoje financovany z verejnych zdroju (s odkazem do CEP)<br>Z - Vyzkumny zamer (s odkazem do CEZ)

Rok uplatnění

2014

Kód důvěrnosti údajů

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

Název periodika

Astrophysical Journal

ISSN

0004-637X

e-ISSN

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Svazek periodika

786

Číslo periodika v rámci svazku

2

Stát vydavatele periodika

US - Spojené státy americké

Počet stran výsledku

6

Strana od-do

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Kód UT WoS článku

000335884500045

EID výsledku v databázi Scopus

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