  Detection of X-ray emission from classical novae in their post-outburst
stages provides crucial information about the nova phenomenon. The soft X-ray
emission gives a direct insight into the remaining hot nuclear burning shell. A
numerical model for steady H-burning white dwarf envelopes has been developed
to study the post-outburst phases of classical novae. Properties of the X-ray
emission of the post-nova white dwarf are obtained, and the results are
compared to ROSAT observations of V1974 Cyg.
