Weighing the White Dwarfs in Symbiotic Stars With X-ray Spectroscopy

Details Weighing the White Dwarfs in Symbiotic Stars With X-ray Spectroscopy Weighing the White Dwarfs in Symbiotic Stars With X-ray Spectroscopy

Sep 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011head...12.1104n&link_type=abstract

American Astronomical Society, HEAD meeting #12, #11.04

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Scientific paper

Recent all sky surveys with Swift and Integral have detected 10-50 keV emission from a small subset of symbiotic stars (white dwarfs accreting material from a red giant companion). These X-rays are thought to originate in the accretion flow, and therefore the high plasma temperatures derived from their X-ray spectra indicate high mass white dwarfs in these systems. I will present new Suzaku observations of the symbiotic stars EG And and 4 Dra aimed at characterizing the X-ray emission in systems with lower mass white dwarfs. These new datasets provide an important test of the X-ray temperature/white dwarf mass diagnostic in symbiotic stars and other accreting white dwarfs, and give insight into the mode of accretion in these systems.

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