Observations and predictions of EUV emission from classical novae
Theoretical modeling of novae in outburst predicts that they should be active emitters of radiation both in the EUV and soft X-ray wavelengths twice during the outburst. The first time is very early in the outburst when only an all sky survey can detect them. This period lasts only a few hours. They again become bright EUV and soft X-ray emitters late in the outburst when the remnant object becomes very hot and is still luminous. The predictions imply both that a nova can remain very hot for months to years and that the peak temperature at this time strongly depends upon the mass of the white dwarf. It is important to observe novae at these late times because a measurement of both the flux and temperature can provide information about the mass of the white dwarf, the tun-off time scale, and the energy budget of the outburst. We review the existing observations of novae in late stages of their outburst and present some newly obtained data for GQ Mus 1983. We then provide results of new hydrodynamic simulations of novae in outburst and compare the predictions to the observations. 43 refs., 6 figs.
- Research Organization:
- Los Alamos National Laboratory (LANL), Los Alamos, NM (United States)
- DOE Contract Number:
- W-7405-ENG-36
- OSTI ID:
- 6399025
- Report Number(s):
- LA-UR-89-494; CONF-890189-1; ON: DE89007984
- Resource Relation:
- Conference: Berkeley colloquium on extreme ultraviolet astronomy, Berkeley, CA, USA, 19 Jan 1989; Other Information: Portions of this document are illegible in microfiche products
- Country of Publication:
- United States
- Language:
- English
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GENERAL PHYSICS
NOVAE
HYDRODYNAMIC MODEL
COMPUTERIZED SIMULATION
EXTREME ULTRAVIOLET SPECTRA
MASS
SOFT X RADIATION
WHITE DWARF STARS
DWARF STARS
ELECTROMAGNETIC RADIATION
ERUPTIVE VARIABLE STARS
IONIZING RADIATIONS
MATHEMATICAL MODELS
PARTICLE MODELS
RADIATIONS
SIMULATION
SPECTRA
STARS
STATISTICAL MODELS
THERMODYNAMIC MODEL
VARIABLE STARS
X RADIATION
640102* - Astrophysics & Cosmology- Stars & Quasi-Stellar
Radio & X-Ray Sources