Post nova white dwarf cooling in V1500 Cygni
M.W. Somers and
Received 26 July 1999 / Accepted 6 October 1999
We use the irradiated secondary star in the remnant of Nova Cyg 1975 as a probe of the cooling white dwarf. At superior conjunction the flux in the B band is dominated by the irradiated face of the secondary star. The heated face produces an orbital modulation which is dependent on the strength of the irradiating source. We demonstrate that the cooling rate of the white dwarf is consistent with the theoretical model of Prialnik (1986).
Key words: stars: binaries: spectroscopic stars: individual: V1500 Cyg stars: novae, cataclysmic variables stars: binaries: close stars: binaries: eclipsing stars: white dwarfs
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© European Southern Observatory (ESO) 1999
Online publication: December 2, 1999