UBVRI polarimetry of AM Herculis-type binaries. 5: The asynchronous (?) polar BY Camelopardalis (H0538+608)

Details UBVRI polarimetry of AM Herculis-type binaries. 5: The asynchronous (?) polar BY Camelopardalis (H0538+608) UBVRI polarimetry of AM Herculis-type binaries. 5: The asynchronous (?) polar BY Camelopardalis (H0538+608)

Mar 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...283..163p&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 283, no. 1, p. 163-174

Astronomy and Astrophysics

Astrophysics

30

Astronomical Polarimetry, Binary Stars, Circular Polarization, Light Curve, Stellar Rotation, White Dwarf Stars, X Ray Sources, Cyclotron Radiation, Ephemeris Time, Linear Polarization, Orbital Mechanics, Stellar Magnetic Fields, Synchronism

Scientific paper

The basic features of the light and circular polarization curves of BY Cam in 1990 Sep can be reproduced by a model with the inclination i = 40-60 deg of the magnetic white dwarf spin axis and two extended emission regions: a strong positive circular polarization region at the colatitude beta = 30-45 deg and a weaker negative circular polarization region at beta = 100-125 deg with a phase lag of about 0.5. The degree of linear polarization was small (approximately less than 1 %), but the observed position angle pattern is roughly consistent with the above geometric picture. However, in November 1990 the reduced amplitude of the position angle curve, and the self-eclipsing-type light curves with distinct bright and faint phases, suggest higher inclination (i approximately 85 deg). Precession with a period of 100-150 days is offered as a hypothetical mechanism for changing the inclination. Timings for the transit of the positive circular polarization region from 1992 Nov and 1993 Jan appear approximately 0.3 phase later than predicted from our linear ephemeris based on data from the time interval JD2446138-8155, indicating a possible period increase of dP/dt approximately 3.3 x 10-4, and a synchronization time scale of approximately 1200 y. This is longer than found for the only well established re-synchronizing magnetic binary V1500 Cyg (approximately 185 y). Further timings are needed to confirm and improve the rotational period of the magnetic white dwarf in BY Cam.

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