Catch me if you can: is there a "runaway-mass" black hole in the Orion Nebula Cluster?

Subr, Ladislav, Kroupa, Pavel and Baumgardt, Holger (2012) Catch me if you can: is there a "runaway-mass" black hole in the Orion Nebula Cluster?. Astrophysical Journal, 757 1: 37.1-37.10. doi:10.1088/0004-637X/757/1/37

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Author Subr, Ladislav
Kroupa, Pavel
Baumgardt, Holger
Title Catch me if you can: is there a "runaway-mass" black hole in the Orion Nebula Cluster?
Journal name Astrophysical Journal   Check publisher's open access policy
ISSN 0004-637X
Publication date 2012-09-01
Year available 2012
Sub-type Article (original research)
DOI 10.1088/0004-637X/757/1/37
Open Access Status File (Publisher version)
Volume 757
Issue 1
Start page 37.1
End page 37.10
Total pages 10
Place of publication Philadelphia, PA, United States
Publisher Institute of Physics Publishing
Language eng
Formatted abstract
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-body interactions 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 in the 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 • ≳ 100 M ⊙). Such a dark object could explain the large velocity dispersion of the four Trapezium stars observed in the ONC core. We further show that the putative massive black hole is likely to be a member of a binary system with ≈70% probability. In such a case, it could be detected either due to short periods of enhanced accretion of stellar winds from the secondary star during pericentre passages, or through a measurement of the motion of the secondary whose velocity would exceed 10 km s -1 along the whole orbit.
Keyword Black hole physics
Stars: kinematics and dynamics
Kinematics and dynamics
Stars: massive
Q-Index Code C1
Q-Index Status Confirmed Code
Grant ID GACR-205/07/0052
Institutional Status UQ
Additional Notes Article number 37

Document type: Journal Article
Sub-type: Article (original research)
Collections: School of Mathematics and Physics
Official 2013 Collection
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Citation counts: TR Web of Science Citation Count  Cited 2 times in Thomson Reuters Web of Science Article | Citations
Scopus Citation Count Cited 1 times in Scopus Article | Citations
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