Astronomy and Astrophysics – Astronomy
Scientific paper
May 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21812713v&link_type=abstract
American Astronomical Society, AAS Meeting #218, #127.13; Bulletin of the American Astronomical Society, Vol. 43, 2011
Astronomy and Astrophysics
Astronomy
Scientific paper
We present the results of time-resolved optical spectroscopy of the classical nova and super-soft X-ray source V723 Cas (Nova Cas 1995). The spectra were obtained at the Steward Observatory Bok 2.3-m telescope (range: 4180-5320 Angstroms) on Kitt Peak and at the MDM Observatory Hilter 2.4-m telescope (range: 4000-7500 Angstroms) in 2007, 2008, and 2010. Both sets of spectra were obtained at a spectral resolution of about 2 Angstroms. Exposure times of the individual spectra were about 20 minutes which is short compared to the 16.6-hour binary orbital period, thus minimizing velocity smearing of spectral features. V723 Cas is an unusual system, being an active super-soft X-ray source for more than 15 years since the 1995 outburst, in contrast to the median X-ray turn off time of only 1.4 years. This may be indicative of steady hydrogen burning on the white dwarf due to renewed accretion (Ness et al. 2008, AJ, 135, 1328). Phasing the individual spectra to the 16.6-hour binary photometric orbital period (Goranskij et al. 2007, Ast. Bull. 62, 125), we find that the Balmer emission lines exhibit a double-peaked accretion disk line profile convolved with a variable Gaussian emission line S-wave component. The He II 4686 emission line exhibits phase-dependent line profile variations as well. We have modeled both emission line profiles with a double-peaked accretion disk line component assuming different disk properties and an independent Gaussian component. The results of our line profile modeling compared to the orbital photometric behavior of V723 Cas are presented and we discuss the interpretation of our synoptic observations in the context of the post-outburst evolution of super-soft X-ray sources and this unusual classical nova.
Hamilton-Drager Catrina
Helton Lorren Andrew
Recine K. A.
Schwarz Gerhard
Vonderharr Thomas
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