Chandra/HETG Spectroscopy Of The Symbiotic Star, CH Cygni, in a High State

Details Chandra/HETG Spectroscopy Of The Symbiotic Star, CH Cygni, in a High State Chandra/HETG Spectroscopy Of The Symbiotic Star, CH Cygni, in a High State

Feb 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010head...11.1906m&link_type=abstract

American Astronomical Society, HEAD meeting #11, #19.06; Bulletin of the American Astronomical Society, Vol. 41, p.689

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The symbiotic star CH Cyg consists of an M giant and a white dwarf, and was the first such object detected as an X-ray source. An ASCA observation revealed it to have a spectacular two-component X-ray spectrum. The strongly absorbed hard X-ray component is likely due to accretion onto the white dwarf, while the unabsorbed soft X-ray component is thought to be either due to colliding winds or due to photoionization of the M giant wind by the hard component. Similar absorbed hard X-ray component has now been discovered in 5 other symbiotic stars, and is interpreted as due to accretion onto massive, non-magnetic white dwarfs, making these objects candidate progenitors of Type Ia supernovae (see also presentations by Luna et al. and by Nelson et al. at this meeting). As to the soft component, CH Cyg remains by far the brightest symbiotic star at 1 keV. All these make CH Cyg an ideal target for a Chandra HETG observation. Unfortunately, several recent X-ray observations (once with Chandra, and twice with Suzaku) have caught it in a low state. We have finally succeeded in obtaining a high state Chandra HETG observation of CH Cyg as a target of opportunity observation, which we triggered based on our on-going RXTE monitoring campaign. We will present the data and our initial interpretations regarding the Fe K-alpha complex, the absorber, and the nature of the soft component, along with variability on time scales of hours and days.

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