Polarimetry of the exceptionally long-period eclipsing polar RX J0515.6+0105

Details Polarimetry of the exceptionally long-period eclipsing polar RX J0515.6+0105 Polarimetry of the exceptionally long-period eclipsing polar RX J0515.6+0105

Aug 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995mnras.275l..61b&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 275, Issue 4, pp. L61-L66.

Astronomy and Astrophysics

Astronomy

22

Accretion, Accretion Discs, Stars: Individual: Rx J0515.6+0105, Stars: Magnetic Fields, Novae, Cataclysmic Variables, White Dwarfs, X-Rays: Stars

Scientific paper

Photopolarimetric observations of RX J0515.6+0105 confirm that this system is a polar (i.e. an AM Herculis system). Circular polarization, varying from -2 to 2 per cent, was measured over an interval of seven nights. Furthermore, a periodogram analysis of the data reveals a 7.99-h period, consistent with the photometrically determined orbital period. This makes RX J0515.6+0105 the longest period polar, exceeding the erstwhile longest period system by ~3.3h. Although the degree of linear polarization is low, there is some evidence for a linear polarization `spike' near orbital phase 0.5, corresponding to when the circular polarization changes sign. Also, the maximum and minimum values of the circular polarization are seen to coincide with the intensity maxima. These characteristics are evidence for two regions of cyclotron emission of differing polarity, and argue in favour of cyclotron beaming as the likely explanation for the prominent humps in the light curves. The near-zero circular polarization at eclipse implies that the cyclotron emitting region is offset from the line of centres of the stars by ~90 deg. The presence of likely cyclotron spectral features implies a magnetic field strength of <~61 MG, which is well below the value inferred from Patterson's synchrontron criterion. This is taken as evidence for a much lower accretion rate than the empirical M_solar(P) relation would imply.

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