Structure and evolution of the globular cluster low mass X-ray binary AC211 in M15

Details Structure and evolution of the globular cluster low mass X-ray binary AC211 in M15 Structure and evolution of the globular cluster low mass X-ray binary AC211 in M15

Jul 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995hst..prop.6026n&link_type=abstract

HST Proposal ID #6026

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Hst Proposal Id #6026 Hot Stars

Scientific paper

AC211 is optically the brightest counterpart of any globular cluster X-ray binary, and one of the brightest amongst all LMXBs. Given its large UV excess and high orbital inclination {evident from its large UV eclipse} this object is a prime target for HST. We are proposing to carry out phase resolved spectrophotometry of AC211 using the temporal and UV spectral resolutions offered by the FOS. We will model the observed eclipses to define the mechanism responsible for the optical and UV luminosity of this system. This is widely believed to be the heating of the accretion disc by X-rays from the corona. A large flux of X-rays scattered down onto the disc produces a large UV luminosity, and thus a flatter radial disc temperature distribution than pure accretion. The behaviour of the spectral lines with orbital phase will allow us to define the geometry of the wind and the accretion disc. The optical line profiles already infer significant mass loss, implying that the UV resonance lines will show phase modulated P Cyg profiles. From these we can estimate the mass loss rate, and hence the mass transfer and wind mechanisms which are related to the evolutionary state of the binary {predicted to be unique to globular clusters}. Only with Space Telescope will we be able to obtain line profiles and continuum measurements which are uncontaminated by light from other cluster members. The results have implications for LMXBs in general and globular cluster X-ray sources in particular.

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