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Photometric variability of the slow nova V723 Cas
We present UBVR photometry of V723 Cas (Nova Cas 1995) obtained fromJanuary 1997 through March 1998. Using these as well as archivalphotoelectric and visual observations, we have found an 180 dayperiodicity of the activity on the declining branch of the light-curve.The stages of activity, characterized by flare(s), occurred after thebrightness decreases. Period analyses of the short-term brightnessvariations and the study of phase light-curves in quiescent stagerevealed the most significant period as 0.63 days. The same analysisapplied on brightness variations in active stage (January-February 1997)revealed the periods 0.61 days or 2.8 days. Detected periods areinterpreted in the frame of possible binary and triple-star models. Theevolutionary path of the nova in the two-colour diagram is presented. Itis shown, that at brightness maximum, discussed as a super-Eddingtonevent, the main envelope of the nova was ejected with the velocity 210km s-1.
| Photometric Study of Nova CAS 1995
We present the results of UBVR photometry of Nova Cassiopeiae 1995obtained in the first 16 months following its outburst. We haveclassified the nova as slow with t3, nu = 173 d, t3,Beta = 189 d. The corresponding absolute magnitudes of the nova atmaximum are MVmax = -6.70 +/- 0.23, MBmax = -6.49+/- 0.32. The latter value yields a mass of 0.66 +/- 0.05 solar mass forthe white dwarf component. We have determined the colour excess E(B-V) =0.57 +/- 0.01 and the distance to the nova d = 2.39 +/- 0.38 kpc.
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