Black Hole Binaries in the LMC

Details Black Hole Binaries in the LMC Black Hole Binaries in the LMC

Jul 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994hst..prop.5711h&link_type=abstract

HST Proposal ID #5711

Physics

Hst Proposal Id #5711

Scientific paper

The endpoints of stellar evolution - white dwarfs, neutron stars and black holes - can be most directly studied when they occur in binary systems such as cataclysmic variables and X-ray binaries. However, only a handful of black-hole candidates have been found, and thus very little is known about their physical properties and associated accretion disks. Two black-hole X-ray binaries, LMC X-3 and CAL 87, are particularly suitable for investigation in the UV, where important diagnostic emission lines are present and where the disk structure can be modelled from the continuum. LMC X-3 has recently been found to have a precessing accretion disk (P = 200 days) allowing different parts of the disk to be observed over a timescale of months. CAL 87 (P orb 10.6hr) is the only known eclipsing black hole, so that observation throughout the eclipse will yield detailed information about the disk structure, particularly very near the collapsed star itself.

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