Other
Scientific paper
Sep 1987
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987mnras.228..389c&link_type=abstract
Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 228, Sept. 15, 1987, p. 389-399. Research supported by
Other
26
Polarimetry, Stellar Luminosity, Stellar Spectrophotometry, Variable Stars, Ephemerides, Light Curve, Orbital Elements, Shock Waves, Stellar Mass Accretion
Scientific paper
Observations of BL Hyi in the bright and faint states are presented. The orbital ephemeris has been updated. The orbital behavior of the polarizations indicates that the accreting pole lies about 27 deg from the rotation axis on the far side of the line-of-sight, and that the system is viewed from slightly above the orbital plane. The bright phase duration is longer than expected and is caused either by the accretion shock being substantially higher above the white dwarf than in the other AM Her systems where this has been determined or by accretion at a second pole. If the former explanation is correct, the asymmetry of the light and polarization curves requires that the shock region varies in height from one edge to the other, or that it is elongated in a direction toward the equator and ahead in phase, or both. The humped nature of the position angle curve also requires an elongation of the shock region toward the equator. If the latter, the accretion region at the second pole is not diametrically opposite that at the first pole, either because the dipole is offset, or accretion is taking place some distance from the magnetic poles, or both.
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