An Evolutionary Model for the Massive Black Hole X-Ray Binary M33 X-7.

Details An Evolutionary Model for the Massive Black Hole X-Ray Binary M33 X-7. An Evolutionary Model for the Massive Black Hole X-Ray Binary M33 X-7.

Sep 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aspc..447..271v&link_type=abstract

Evolution of compact binaries. Proceedings of a workshop held at Hotel San Martín, Viña del Mar, Chile 6–11 May 2011. ASP Confe

Astronomy and Astrophysics

Astronomy

Scientific paper

Black hole (BH) X-ray binaries (XRBs) are X-ray bright binary systems comprising a BH accreting matter from a companion star. Unravelling the evolutionary history of observed XRBs can shed light on how BHs form, evolve and interact with their host environment, processes that yet lack a conclusive physical explanation. Our focus here lies on M33 X-7, which is among the heaviest BH XRBs known to date, hosting a 15.65 M&sun; BH orbiting a 70 M&sun; companion star in a 3.45 day orbit. The high masses of the binary components and the tight orbit present a challenge for typically invoked BH-XRBs formation channels. The picture is further complicated by the measured underluminosity of the stellar component. Here we propose the first evolutionary scenario for M33 X-7 that is consistent with the complete set of current observational constraints. According to our model, the progenitors of M33 X-7 are constrained to host primaries and secondaries between 85-99 M&sun; and 28-32 M&sun;, respectively, and initial orbital periods between 2.8-3.1 days. In order to form a BH of 15.65 M&sun;, the BH progenitor transferred part of its envelope to the companion star and lost the rest in a strong stellar wind. During this dynamically stable mass transfer phase the companion accreted matter, to become the presently underluminous 70 M&sun; star.

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