The Ultraviolet Emission from Magnetic Variables

Details The Ultraviolet Emission from Magnetic Variables The Ultraviolet Emission from Magnetic Variables

Jul 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991hst..prop.2686s&link_type=abstract

HST Proposal ID #2686

Computer Science

Hst Proposal Id #2686

Scientific paper

We propose to use the time-resolved spectroscopy mode of the FOS to study the origins of UV emission in the AM Her-type or magnetic variables. Since the magnetic variables are "naked" (they have no obscuring or diluting accretion disk), they have proved to be invaluable in increasing our understanding of cataclysmic variables and accretion binaries. While these systems are relatively well understood in a qualitative sense, the origin of the UV "upturn" around 1250-1500A is still a major mystery. When first discovered in AM Her by IUE, this flux was interpreted as either evidence for steady nuclear burning or direct energy deposition into the accreting white dwarf photosphere. The implied luminosities, L ~10E35 erg/s, are several orders of magnitude greater than observed in hard X-ray or optical bands. While several theories address this "soft X-ray/UV" excess, we propose to establish the size and positions of the emission regions using HST observations of eclipses by the red companion and the W.D. itself.

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