Computer Science
Scientific paper
Jul 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993hst..prop.4449m&link_type=abstract
HST Proposal ID #4449
Computer Science
Hst Proposal Id #4449
Scientific paper
One of the fundamental and outstanding problems to be resolved in AM Her stars is the origin of the high ratio of the soft/hard X-ray flux ratio compared to the value (~ 1) predicted in the conventional shock model. The only explanation so far advanced is that of a `blobby' accretion flow which directly penetrates and heats the white dwarfs photosphere, thereby enhancing the soft X-ray flux at the expense of the hard X-ray flux. Clearly, knowledge of the state of the gas near the white dwarf is crucial in trying to understand this problem. We propose to probe the structure of the inner, UV emitting accretion stream in RE1149+28, the most extreme example of a EUV bright system. RE1149+28 has the highest EUV/optical ratio of any known AM Her, and therefore it might be expected that most of the accretion occurs via blobs. By studying the UV line emission in RE1149+28 we can gain critical information on the gas close into the WD surface, such a study being facilitated by that fact that RE1149+28 is a pole occulting system. The structure of the accretion stream can therefore be observed as it crosses the limb of the white dwarf.
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