Evolution of the post-nova GQ MUS (Nova MUSCAE 1983). II. Stellar atmospheres, coronal lines, and turnoff.

Details Evolution of the post-nova GQ MUS (Nova MUSCAE 1983). II. Stellar atmospheres, coronal lines, and turnoff. Evolution of the post-nova GQ MUS (Nova MUSCAE 1983). II. Stellar atmospheres, coronal lines, and turnoff.

Sep 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996a%26a...313..611m&link_type=abstract

Astronomy and Astrophysics, v.313, p.611-623

Astronomy and Astrophysics

Astrophysics

3

Atomic Data, Stars: Individual: Gq Mus, Stars: Novae, Interstellar Medium: General, Planetary Nebulae: General

Scientific paper

Photoionization models for the shell ejected by Nova Muscae 1983 are obtained for the period 1984-1992, considering post-nova atmosphere continua computed by MacDonald & Vennes (1991). A fit to their grid of models is proposed in an appendix. All features of the model shell obtained by Morisset & Pequignot assuming a blackbody primary source are preserved. However the effective temperature T_*_ derived for the source is about 15% lower. Reliable collision strengths for coronal lines are needed before the late evolution of the post-nova can be accurately determined. An extensive exploration of possible photoionization-model solutions indicates that (1) a suitable effective collision strength {OMEGA}_X_ for [Fe X] 637.5nm at 2x10^4^K is 3 to 5 times the pioneering result of Blaha (1969) and less than one half recent elaborate values, which are therefore strongly suspected to be overestimated, (2) the collision strength for [S VIII] 991.1 is moderately larger than according to Blaha, (3) the decline of the bolometric luminosity L_*_ amounts to a factor ~2 at the time of soft X-ray detection by ROSAT (day 3330), which may therefore nearly coincide with nuclear burning turnoff and maximum T_*_, and (4) depending on the collision strength {OMEGA}_XI_ for [Fe XI] 789.2nm, the maximum T_*_ is either of the order of 5x10^5^K ({OMEGA}_XI_ close to Blaha's result) or smaller than 4x10^5^K (large {OMEGA}_XI_). A way out of the conflict between theoretical and astrophysical determinations of {OMEGA}_X_ may be managed in the framework of present models if {OMEGA}_XI_ happens to be very large. Source parameters derived from nova shell models are relatively insensitive to details of stellar atmosphere models and may help to enhance the value of soft X-ray observations. Properties of GQ Mus disclosed by photoionization model analysis are shown to constitute a challenge to current understanding of novae and post-novae.

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