Unravelling the Puzzle of the Eclipsing Polar SDSSJ 015543.40+002807.2 with XMM and Optical Photometry/Spectropolarimetry

Details Unravelling the Puzzle of the Eclipsing Polar SDSSJ 015543.40+002807.2 with XMM and Optical Photometry/Spectropolarimetry Unravelling the Puzzle of the Eclipsing Polar SDSSJ 015543.40+002807.2 with XMM and Optical Photometry/Spectropolarimetry

2004-10-12

arxiv.org/abs/astro-ph/0410320v1

Astrophys.J. 620 (2005) 422-431

Astronomy and Astrophysics

Astrophysics

20 pages, 12 figures

Scientific paper

10.1086/426807

The cataclysmic variable SDSSJ 015543.40+002807.2 is confirmed to be a magnetic system of the AM Herculis type. With an orbital period of 87.13 min, it is also the shortest-period eclipsing Polar known. Monitoring with XMM-Newton finds a high-state light curve dominated by a single X-ray emitting accretion pole located slightly prograde of the secondary star. The hard X-ray spectrum is typical of radial shocks on magnetic white dwarfs (kT ~ 10keV), and there is evidence for a soft X-ray component consistent with reprocessing from the stellar surface. The optical circular polarization is weak (v < 3%) when the accretion rate is high (mV ~ 15.5), due to optically-thick cyclotron emission and the apparent competition between two accreting poles. However, in low states (mV ~ 18), the polarization increases smoothly to the blue, reaching 20% at 4200A, and the flux spectrum displays a rich set of thermally-broadened cyclotron harmonics that indicate a polar field of 29MG. The phase interval preceding the 6.5 min eclipse depicts the development of P-Cygni components followed by complete absorption reversals in the emission lines. This phenomenon is not unexpected for a strongly accreting magnetic system viewed through the cool base of the funnel, and high-quality spectroscopy through this interval will likely lead to new insights into the dynamics of magnetic coupling and gas flow onto the white dwarf.

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