Dynamics of star associations in an SMBH-IMBH system: The case of IRS13 in the Galactic centre

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F24%3A00603209" target="_blank" >RIV/67985815:_____/24:00603209 - isvavai.cz</a>

Výsledek na webu

<a href="https://hdl.handle.net/11104/0361024" target="_blank" >https://hdl.handle.net/11104/0361024</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1051/0004-6361/202452050" target="_blank" >10.1051/0004-6361/202452050</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Dynamics of star associations in an SMBH-IMBH system: The case of IRS13 in the Galactic centre

Popis výsledku v původním jazyce

Context. The existence of intermediate-mass black holes (IMBHs) still poses challenges to theoretical and observational astronomers. Several candidates have been proposed, including the one in the IRS13 cluster in the Galactic centre, where the evidence is based on the velocity dispersion of its members, however, none have been confirmed to date. Aims. We aim to gain insights into the presence of an IMBH in the Galactic centre through a numerical study of the dynamical interplay between an IMBH and star clusters (SCs) in the vicinity of a supermassive black hole (SMBH). Methods. We used high-precision N-body models of IRS13-like SCs in the Galactic centre, and of more massive SCs that fall into the centre of the Galaxy from larger distances. Results. We find that at IRS13's physical distance of 0.4 pc, an IRS13-sized SC cannot remain gravitationally bound even if it contains an IMBH of thousands of M circle dot. Thus, IRS13 appears to be an incidental present-day clumping of stars. Furthermore, we show that the velocity dispersion of tidally disrupted SCs (the likely origin of IRS13) can be fully accounted for by the tidal forces of the central SMBH, the IMBH's influence is not essential.

Název v anglickém jazyce

Dynamics of star associations in an SMBH-IMBH system: The case of IRS13 in the Galactic centre

Popis výsledku anglicky

Context. The existence of intermediate-mass black holes (IMBHs) still poses challenges to theoretical and observational astronomers. Several candidates have been proposed, including the one in the IRS13 cluster in the Galactic centre, where the evidence is based on the velocity dispersion of its members, however, none have been confirmed to date. Aims. We aim to gain insights into the presence of an IMBH in the Galactic centre through a numerical study of the dynamical interplay between an IMBH and star clusters (SCs) in the vicinity of a supermassive black hole (SMBH). Methods. We used high-precision N-body models of IRS13-like SCs in the Galactic centre, and of more massive SCs that fall into the centre of the Galaxy from larger distances. Results. We find that at IRS13's physical distance of 0.4 pc, an IRS13-sized SC cannot remain gravitationally bound even if it contains an IMBH of thousands of M circle dot. Thus, IRS13 appears to be an incidental present-day clumping of stars. Furthermore, we show that the velocity dispersion of tidally disrupted SCs (the likely origin of IRS13) can be fully accounted for by the tidal forces of the central SMBH, the IMBH's influence is not essential.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

—

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

Astronomy & Astrophysics

ISSN

0004-6361

e-ISSN

1432-0746

Svazek periodika

692

Číslo periodika v rámci svazku

Dec.

Stát vydavatele periodika

FR - Francouzská republika

Počet stran výsledku

8

Strana od-do

A104

Kód UT WoS článku

001379065700007

EID výsledku v databázi Scopus

2-s2.0-85212922639