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- W2077777545 abstract "We present U and B photometry, based on Hubble Space Telescope observations, for 26 stars in the R136 region of the young cluster 30 Doradus in the Large Magellanic Cloud. It has been suggested that rich star clusters form through the coalescence of clumps, and it seems likely that the R136 region is such a clump. If it is in virial equilibrium then its mass (|$sim 1500enspace M_odot$|) and radius (∼0.8 pc) imply a velocity dispersion of ∼ 3 km s−1. The three brightest stars in the clump may have masses as large as |$sim 250enspace M_odot$|, but given the uncertainties, a value this large is not required by the data. Two of these stars have a projected separation of only ∼ 4500 AU, and may constitute a hard binary with orbital velocity ∼ 12.5 ± 1.5 km s−1. N-body simulations suggest that mass loss through stellar evolution would unbind the clump after only a few million years, and that it is unlikely that a hard binary could form dynamically in that time. We therefore conclude that, if the two massive stars are a binary, it is primordial." @default.
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- W2077777545 date "1992-09-01" @default.
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- W2077777545 title "The massive stars in the R136 region of 30 Doradus" @default.
- W2077777545 doi "https://doi.org/10.1093/mnras/258.1.103" @default.
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