CATCH ME IF YOU CAN: IS THERE A "RUNAWAY-MASS" BLACK HOLE IN THE ORION NEBULA CLUSTER?

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F12%3A10129560" target="_blank" >RIV/00216208:11320/12:10129560 - isvavai.cz</a>

Výsledek na webu

<a href="http://dx.doi.org/10.1088/0004-637X/757/1/37" target="_blank" >http://dx.doi.org/10.1088/0004-637X/757/1/37</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1088/0004-637X/757/1/37" target="_blank" >10.1088/0004-637X/757/1/37</a>

Jazyk výsledku

angličtina

Název v původním jazyce

CATCH ME IF YOU CAN: IS THERE A "RUNAWAY-MASS" BLACK HOLE IN THE ORION NEBULA CLUSTER?

Popis výsledku v původním jazyce

We investigate the dynamical evolution of the Orion Nebula Cluster (ONC) by means of direct N-body integrations. A large fraction of residual gas was probably expelled when the ONC formed, so we assume that the ONC was much more compact when it formed compared with its current size, in agreement with the embedded cluster radius-mass relation from Marks & Kroupa. Hence, we assume that few-body relaxation played an important role during the initial phase of evolution of the ONC. In particular, three-bodyinteractions among OB stars likely led to their ejection from the cluster and, at the same time, to the formation of a massive object via "runaway" physical stellar collisions. The resulting depletion of the high-mass end of the stellar mass function inthe cluster is one of the important points where our models fit the observational data. We speculate that the runaway-mass star may have collapsed directly into a massive black hole (M center dot greater than or similar to 100 M-circle do

Název v anglickém jazyce

CATCH ME IF YOU CAN: IS THERE A "RUNAWAY-MASS" BLACK HOLE IN THE ORION NEBULA CLUSTER?

Popis výsledku anglicky

We investigate the dynamical evolution of the Orion Nebula Cluster (ONC) by means of direct N-body integrations. A large fraction of residual gas was probably expelled when the ONC formed, so we assume that the ONC was much more compact when it formed compared with its current size, in agreement with the embedded cluster radius-mass relation from Marks & Kroupa. Hence, we assume that few-body relaxation played an important role during the initial phase of evolution of the ONC. In particular, three-bodyinteractions among OB stars likely led to their ejection from the cluster and, at the same time, to the formation of a massive object via "runaway" physical stellar collisions. The resulting depletion of the high-mass end of the stellar mass function inthe cluster is one of the important points where our models fit the observational data. We speculate that the runaway-mass star may have collapsed directly into a massive black hole (M center dot greater than or similar to 100 M-circle do

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

—

Návaznosti

Z - Vyzkumny zamer (s odkazem do CEZ)

Rok uplatnění

2012

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

—

Svazek periodika

757

Číslo periodika v rámci svazku

1

Stát vydavatele periodika

US - Spojené státy americké

Počet stran výsledku

10

Strana od-do

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Kód UT WoS článku

000309052800037

EID výsledku v databázi Scopus

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