Abstract

SS Cyg is a dwarf nova binary star that undergoes frequent large amplitude outburst within a period of 40 days. SS Cyg was observed with the Chandra x-ray telescope in quiescence on 2000 August 24, and near the peak and early decline of a narrow outburst on 2000 September 12 and 14 (exposures of 47 and 96 ks). The spectrum of the source shows strong emission lines of O VII and O VIII in all three observations. These lines, we note, originate from the boundary layer.

DOI

Keywords

Cataclysmic Variables, emission lines, SS Cyg, dwarf novas

First Page

227

Last Page

229

Recommended Citation

EZE, ROMANUS N. C. (2007) "The Origin of X-Ray Emission Lines From SS Cgy," Turkish Journal of Physics: Vol. 31: No. 4, Article 7. Available at: https://journals.tubitak.gov.tr/physics/vol31/iss4/7

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