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V1974 Cyg (Nova Cyg 1992) - A Possible Link to SU Uma Stars

Published online by Cambridge University Press:  12 April 2016

A. Retter ,
E. M. Leibowitz  and
E. O. Ofek
A. Retter
Affiliation:
Tel-Aviv University, Israel
E. M. Leibowitz
Affiliation:
Tel-Aviv University, Israel
E. O. Ofek
Affiliation:
Tel-Aviv University, Israel

Extract

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V1974 Cyg erupted on 1992 February 19, and was the brightest nova since V1500 Cyg. It soon became an object of massive international multiwavelength observational study.

Some major photometric features of the nova were investigated by DeYoung & Schmidt (1994), and Semeniuk et al. (1994,1995). They found two periodicities in the nova light curve. While the shorter 0.081263 d period was present during the 1993 and 1994 observations, the longer 0.0850 d period was only observed from 1994 July. Semeniuk et al. (1995) interpreted the shorter period as the orbital period of the binary system, and the longer one as caused by the rotation of the white dwarf due to a magnetic field.

Type
Novae & Symbiotic Stars
Information
International Astronomical Union Colloquium , Volume 158: Cataclysmic Variables and Related Objects , 1996 , pp. 321 - 322
Copyright
Copyright © Kluwer 1996

References

DeYoung, J.A., Schmidt, R.E., 1994, Ap. J., 431, L47 Google Scholar
la Dous, C., 1993, in “Cataclysmic Variables & Related Objects”, ed. Hack, M., la Dous, C., Centre National de la Recherce Scientifique, Paris, France, p 49 Google Scholar
Semeniuk, I., Pych, W., Olech, A., Ruszkowski, M., 1994, Acta Astron., 44, 277 Google Scholar
Semeniuk, I., DeYoung, J.A., Pych, W., et al., 1995, Acta Astron., 45, 365 Google Scholar
Stolz, B., Schoembs, R., 1981, IBVS 2029 Google Scholar
Stolz, B., Schoembs, R., 1984, A&A, 132, 187 Google Scholar