X-Ray/Optical Studies of Two Outbursts of the Intermediate Polar YY (DO) Draconis

Details X-Ray/Optical Studies of Two Outbursts of the Intermediate Polar YY (DO) Draconis X-Ray/Optical Studies of Two Outbursts of the Intermediate Polar YY (DO) Draconis

Jan 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aj....123..413s&link_type=abstract

The Astronomical Journal, Volume 123, Issue 1, pp. 413-419.

Astronomy and Astrophysics

Astronomy

17

Stars: Novae, Cataclysmic Variables, Stars: Individual: Constellation Name: Yy Draconis, Stars: Individual (Do Draconis), X-Rays

Scientific paper

YY Draconis (likely the same variable called DO Draconis) is one of a small number of intermediate polars (IPs) that show outburst behavior. We report results from Target of Opportunity observations with the Rossi X-Ray Timing Explorer, together with ground-based optical photometry during outbursts in 1999 September and 2000 November. Similar behavior was evident in both outbursts. At outburst, the X-ray flux increased by more than a factor of 12, and the spectrum became hotter and more absorbed compared to quiescence. While the spin pulse at 529 s is clearly present in the X-ray data at 2-4 days past outburst peak and during quiescence, it was not detected in the X-ray data closest to outburst (1.5 days). This is contrary to the large increase in spin pulse amplitude that has been seen during outbursts of the IPs GK Per, XY Ari, and EX Hya. The differences in YY Dra are likely due to its unique geometry, with two relatively equal poles located near the white dwarf equator. The equal enhancement of both poles near outburst could account for the low pulse amplitude, while unequal feeding of the poles as the magnetosphere recedes during decline could explain the changes in amplitude and pulse shape. The changing height of the shocks may also have an effect on the visibility of both poles.

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