The Evolution And Nature Of The Classical Nova And Super-Soft X-ray Source CSS081007:030559+054715

Details The Evolution And Nature Of The Classical Nova And Super-Soft X-ray Source CSS081007:030559+054715 The Evolution And Nature Of The Classical Nova And Super-Soft X-ray Source CSS081007:030559+054715

Jan 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21541623w&link_type=abstract

American Astronomical Society, AAS Meeting #215, #416.23; Bulletin of the American Astronomical Society, Vol. 42, p.269

Astronomy and Astrophysics

Astronomy

Scientific paper

The unusual high galactic latitude transient source CSS081007:030559+054715 was discovered by the Catalina Real-Time Transient Survey on 2008 Oct 7. Early optical spectra revealed strong and broad (HWZI 3100 km/s) emission lines of H I, He II, [O III], [Ne III], [Ne IV], and [Ne V] similar to those observed in some classical novae which may originate on ONeMg white dwarfs. In 2008 November a strong and variable soft X-ray source coincident with CSS081007 was detected by Swift in both the XRT and UVOT bands. Subsequent monitoring by Swift revealed the presence of a 1.77-day periodicity, visible in both the X-ray and UV bands, which might be related to the orbital period of the underlying binary system. Observations in early 2009 by Swift showed a significant decline in X-ray and UV flux. Contemporaneous optical spectra obtained between 2008 December and 2009 August showed fading broad emission lines from the nebular ejecta and weaker narrower emission lines of H I, He II, and O VI superposed on a strong blue continuum. During the outburst, the Hα line profile exhibited three well-resolved and variable emission line components. Comparisons of CSS081007 to classical novae and persistent super-soft X-ray sources such as Cal 83 will be presented and discussed.

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