Runaway massive stars from R136: VFTS 682 is very likely a "slow runaway"

Details Runaway massive stars from R136: VFTS 682 is very likely a "slow runaway" Runaway massive stars from R136: VFTS 682 is very likely a "slow runaway"

2011-11-01

arxiv.org/abs/1111.0291v1

Astronomy and Astrophysics

Astrophysics

Galaxy Astrophysics

21 pages (AASTeX preprint format), 4 figures, 4 tables, 2 online tables. Accepted for publication in The Astrophysical Journal

Scientific paper

We conduct a theoretical study on the ejection of runaway massive stars from R136 --- the central massive, star-burst cluster in the 30 Doradus complex of the Large Magellanic Cloud. Specifically, we investigate the possibility of the very massive star (VMS) VFTS 682 being a runaway member of R136. Recent observations of the above VMS, by virtue of its isolated location and its moderate peculiar motion, have raised the fundamental question whether isolated massive star formation is indeed possible. We perform the first realistic N-body computations of fully mass-segregated R136-type star clusters in which all the massive stars are in primordial binary systems. These calculations confirm that the dynamical ejection of a VMS from a R136-like cluster, with kinematic properties similar to those of VFTS 682, is common. Hence the conjecture of isolated massive star formation is unnecessary to account for this VMS. Our results are also quite consistent with the ejection of 30 Dor 016, another suspected runaway VMS from R136. We further note that during the clusters' evolution, mergers of massive binaries produce a few single stars per cluster with masses significantly exceeding the canonical upper-limit of 150 solar mass. The observations of such single super-canonical stars in R136, therefore, do not imply an IMF with an upper limit greatly exceeding the accepted canonical 150 solar mass limit, as has been suggested recently, and they are consistent with the canonical upper limit.

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