The X-ray spectral evolution of classical Nova V1974 Cygni 1992: A reanalysis of the ROSAT data

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Balman S., Krautter J., Ogelman H.

ASTROPHYSICAL JOURNAL, vol.499, no.1, pp.395-406, 1998 (SCI-Expanded) identifier identifier

  • Publication Type: Article / Article
  • Volume: 499 Issue: 1
  • Publication Date: 1998
  • Doi Number: 10.1086/305600
  • Journal Indexes: Science Citation Index Expanded (SCI-EXPANDED), Scopus
  • Page Numbers: pp.395-406
  • Keywords: binaries, close, novae, cataclysmic variables, radiation mechanisms, thermal, stars, abundances, stars, individual (Nova V1974 Cygni), X-rays, stars, ACCRETING WHITE-DWARFS, RECURRENT NOVAE, CNO ABUNDANCES, HERCULIS 1991, NEON NOVA, EMISSION, OUTBURST, NOVA-CYGNI-1992, MODEL, SHELL
  • Middle East Technical University Affiliated: Yes


We present a spectral analysis of the archival X-ray data of classical Nova V1974 Cygni 1992 (Nova Cygni 1992) obtained by the ROSAT Position Sensitive Proportional Counter (PSPC). The X-ray spectrum is fitted with a two-component model. The first component is a white dwarf atmosphere emission model developed for the remnants of classical novae near the Eddington luminosity. The model is used to fit the soft X-ray data in the similar to 0.1-1.0 keV range, where the bulk of emission is below 0.7 keV. The second component is a Raymond-Smith model of thermal plasma applied to the hard X-ray emission above similar to 1.0 keV. The postoutburst X-ray spectrum of the remnant white dwarf is examined in the context of evolution on the Hertzsprung-Russell diagram using an O-Ne- and a C-O-enhanced atmosphere emission model. A constant bolometric luminosity evolution is detected with increasing effective temperature and decreasing photospheric radius using the O-Ne-enhanced model. The unabsorbed soft X-ray flux for the constant bolometric luminosity phase is found to be in the range (1.7-2.2) x 10(-7) ergs s(-1) cm(-2). A peak effective temperature of 51 eV (5.9 x 10(5) K) is detected 511 days after outburst. We also present the spectral development of the hard X-ray component. It is found to evolve independently of the soft one. The maximum of the hard X-ray emission is reached at similar to 150 days after outburst with an unabsorbed flux of similar to 2.0 x 10(-11) ergs s(-1) cm(-2) corresponding to a luminosity of (0.8-2.0)x 10(34) ergs s(-1) at a 2-3 kpc source distance. The time evolution of the hard X-ray flux and the plasma temperatures decreasing from 10 keV to 1 keV suggest emission from shock-heated gas as the origin of the hard X-ray component.