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Scientific paper
Jul 1999
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999hst..prop.8156h&link_type=abstract
HST Proposal ID #8156
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Hst Proposal Id #8156 Binary Stars
Scientific paper
The intermediate polars {IPs} show several types of behavior. Some show only hard bremsstrahlung X-ray spectra, while others show an additional soft black-body component. Some show quasi- sinusoidal single-peaked pulses at the white dwarf spin period, others show double-peaked pulse profiles. We have suggested that both dichotomies are related to the area of the accretion footprint on the white dwarf, and hence to the process by which the magnetic field disrupts the accretion disk. In order to confirm or refute our hypothesis we aim to observe V405 Aur, the only IP showing both a soft X-ray component and a double-peaked pulse profile. We will use UV STIS spectra to measure the temperature of the pulsation, and hence deduce its emitting area {one of the most useful pieces of information to obtain, since it can be immediately compared to the white dwarf area to tell us where the pulse originates}. We will further compare the UV pulse profile to the optical and X-ray pulse profiles and model all three with our simulation code to deduce their origin. Additionally, the analysis of the UV line profiles will give us velocity information from near the white dwarf for the first time. By putting all this information together we can deduce the accretion geometry, and thus, by tracing field lines back to the point where the field disrupts the disk, obtain constraints on the {largely unknown} physics of the transition region.
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