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V 1500 Cyg: Slow Variability in Post-nova Stage

Published online by Cambridge University Press:  12 April 2016

E. Pavlenko
E. Pavlenko*
Affiliation:
Crimean Astrophysical Observatory, 334413 p/o Nauchny, Crimea, USSR

Extract

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Regular photometric observations of V1500 Gyg (Nova Cygni 1975) have been carried out at the Crimean Astrophysical Observatory of the USSR Academy of Sciences from 1975 till now. The 0.5 m telescope equipped with a TV system is used to estimate the star brightness in V.

The decline of the mean brightness is presented in Figure 1. The solid lines (1) and (2) show the changes of the V brightness according to Patterson (1979) and Arkhipova and Zaitseva (1978), respectively. The dotted line is drawn according to our data (Pavlenko 1988). The arrows indicate the amplitudes of the light and colour variations.

Type
1a. Basic Properties of Novae
Information
International Astronomical Union Colloquium , Volume 122: Physics of Classical Novae , 1990 , pp. 68 - 70
Copyright
Copyright © Springer-Verlag 1990

References

Patterson, J.:1979, Astrophys. J., 131. 789.CrossRefGoogle Scholar
Arkhipova, V.P. and Zaitseva, G.V.:1978, Astron. Tsirk., 1005, 4 Google Scholar
Pavlenko, E.P.:1988, Bull. Crimean Astrophys. Obs., 79, 103.Google Scholar
Abramenko, A.N. and Pavlenko, E.P.:1983, Bull. Crimean Astrophys. Obs. 66, 183.Google Scholar
Pavlenko, E.P., Pelt, J.:1988, JBVS, No. 3252.Google Scholar
Stockman, H.S., Schmidt, G.D., Lamb, D.Q.:1988, Astrophys. J., 1 Google Scholar