Energy Balance and Emission Lines in DQ Herculis - Cycle 3, Medium

Details Energy Balance and Emission Lines in DQ Herculis - Cycle 3, Medium Energy Balance and Emission Lines in DQ Herculis - Cycle 3, Medium

Jul 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993hst..prop.4589p&link_type=abstract

HST Proposal ID #4589

Computer Science

Hst Proposal Id #4589

Scientific paper

The accretion flows onto the magnetic white dwarfs in DQ Herculis stars are only dimly understood. Rapid rotation of the white dwarfs is signified by the presence of pulsations, but the flux in the observed pulses is small compared to that of the disk light, contrary to theory. We propose to use the continuum channels in the FOS to look for large-amplitude pulses in the UV light of YY Dra, and thereby constrain the flux and temperature associated with the accretion bright spot (presumably beneath the radial accretion shock.) We also propose to look for a wavelength-dependent phase shift across the strong UV emission lines, which would be indicative of an ionizing searchlight beam sweeping in azimuth around the disk. This would conclusively certify a photoionization origin for the UV lines, and the phase would decide between origin in an accretion column or a disk.

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