The analyses of X-ray emission from classical novae during the outburst stage have shown that the soft X-ray emission below 1 keV , which is thought to originate from the photosphere of the white dwarf , is inconsistent with the simple blackbody model of emission .
Thus , ROSAT Position Sensitive Proportional Counter ( PSPC ) archival data of the classical novae GQ Mus 1983 ( GQ Mus ) have been reanalyzed in order to understand the spectral development in the X-ray wavelengths during the outburst stage .
The X-ray spectra are fitted with the hot white dwarf atmosphere emission models developed for the remnants of classical novae near the Eddington luminosity .
The post-outburst X-ray spectra of the remnant white dwarf is examined in the context of evolution on the Hertzsprung-Russell diagram using C-O enhanced atmosphere models .
The data obtained in 1991 August ( during the ROSAT All Sky Survey ) indicate that the effective temperature is kT _ { e } < 54 eV ( < 6.2 \times 10 ^ { 5 } K ) .
The 1992 February data show that the white dwarf had reached an effective temperature in the range 38.3-43.3 eV ( 4.4-5.1 \times 10 ^ { 5 } K ) with an unabsorbed X-ray flux ( i.e. , \sim bolometric flux ) between 2.5 \times 10 ^ { -9 } and 2.3 \times 10 ^ { -10 } erg s ^ { -1 } cm ^ { -2 } .
We show that the H burning at the surface of the WD had most likely ceased at the time of the X-ray observations .
Only the 1991 August data show evidence for ongoing H burning .