Probing the 230 MG Accreting Magnetic White Dwarf in AR Ursae Majoris

Details Probing the 230 MG Accreting Magnetic White Dwarf in AR Ursae Majoris Probing the 230 MG Accreting Magnetic White Dwarf in AR Ursae Majoris

Dec 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997hst..prop.7397s&link_type=abstract

HST Proposal ID #7397

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Hst Proposal Id #7397 Binary Stars

Scientific paper

During the past year we identified the luminous X-ray source AR UMa to be the first ``high-field'' {B > 100 MG} AM Her- type magnetic accretion binary. Evidence for a strong magnetic field on the primary star comes from several lines of evidence, however the quantitative estimate of B 230 MG is based on the identification of the photospheric LyAlpha Sigma+ Zeeman component with an absorption feature in the low-state IUE spectrum, which itself is of limited S/N and offers no binary phase resolution. We propose to place this discovery on a firmer observational footing through low- resolution, phase-resolved FUV and NUV spectroscopy with STIS. Two detector/grating combinations will 1} examine the position and shape of the LyAlpha Sigma+ feature at high S/N throughout the orbital cycle; 2} enable a search for the LyAlpha PI component, which is expected to appear just shortward of the geocoronal line at this field strength; 3} evaluate the reality of other Zeeman features suggested by the current data; and 4} allow the emitted energy distribution to be compared to lower-field AM Her systems being studied with HST. Already, the peculiar properties of AR UMa suggest that the dyamics and radiation physics of accreted material in high-field binaries are qualitatively different from the standard AM Her systems, and therefore that study of high-field objects will lend new insight into the general phenomenon of accretion in strong magnetic fields.

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