The Case for a Black Hole in BM Orionis

Details The Case for a Black Hole in BM Orionis The Case for a Black Hole in BM Orionis

Nov 1972

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1972ap%26ss..19..165w&link_type=abstract

Astrophysics and Space Science, Volume 19, Issue 1, pp.165-171

Astronomy and Astrophysics

Astrophysics

12

Scientific paper

Earlier photometric and spectroscopic observations of the binary BM Ori are interpreted in terms of a thin disk model for the object which causes the eclipses. It is shown that the secondary mass, about which the disk particles orbit, has small dimensions and a mass of 3 to 4m &sun;, which suggests that it can only be a collapsed star. The model requires a history of mass exchange or mass loss for the binary. If the Trapezium stars have been formed with the past 2×104 yr, as some studies have indicated, a less conventional alternative, perhaps involving fragmentation of a pre-stellar mass, is needed. Further observations may make it possible to decide for certain between this and a recent model by Hall.

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