The massive stars in the R136 region of 30 Doradus

Details The massive stars in the R136 region of 30 Doradus The massive stars in the R136 region of 30 Doradus

Sep 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992mnras.258..103e&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 258, no. 1, Sept. 1, 1992, p. 103-106.

Astronomy and Astrophysics

Astronomy

11

Binary Stars, Magellanic Clouds, Massive Stars, Star Clusters, Stellar Spectrophotometry, Color-Magnitude Diagram, Hubble Space Telescope, Star Distribution, Stellar Evolution

Scientific paper

We present U and B photometry, based on HST observations, for 26 stars in the R136 region of the young cluster 30 Doradus in the LMC. It seems likely that the R136 region is a clump. If it is in virial equilibrium then its mass and radius imply a velocity dispersion of about 3 km/s. Two of these stars have a projected separation of only about 4500 AU, and may constitute a hard binary with orbital velocity about 12.5 +/- 1.5 km/s. 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.

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