Thermal X-ray emission from classical novae in optical decline

Abstract

Observations of soft X-rays emitted by the hot stellar remnant of classical nova outbursts provide a means of probing the late stage of the evolution of the remnant. Determination of the rate of evolution of the remnant may discriminate between theoretical ideas of how mass is lost from the nova envelope during optical decline and provide an estimate of the white-dwarf mass that is independent of the distance. As a step in this direction, model atmosphere calculations are presented of the X-ray emission from the photospheres of hot, high-gravity stars, which can be used to interpret forthcoming Rosat data.