Recent and Future X-ray Observations of Classical Novae During the Outburst Stage

Abstract

The discovery of soft X-rays from Nova GQ Mus with the EXOSAT satellite has added an important channnel to the observational information on classical novae during the outburst stage (Ögelman, Beuermann, and Krautter 1984). With peak luminosities in excess of 1038 erg s−1 and total liberated energies of more than 1045 erg, novae constitute the second most energetic outburst phenomena in the galactic population exceeded only by supernovae (see Gallagher and Starrfield, 1978; Truran, 1982 for a review of the observations and theory). Regardless of the details of the outburst, objects of the size of white dwarfs (~ 109 cm) radiating close to Eddington luminosities (~ 1038 erg s−1 ) should emit soft X-rays provided that the envelope is sufficiently transparent. In addition, the ejected shell, moving at velocities around 1000 km s−1, is capable of shocking the circumstellar medium to X-ray temperatures.