Photometric and photographic observations of the long-period variable VV Cephei at the time of its eclipse from 1976 to 1978 are reported. The photoelectric standard UBV observations and photographic R(o)I(o) observations reveal the usual semiregular variations and a short-period flickering in U light. Evaluation of the contact times in B and U indicates that the duration of totality is much shorter than predicted, while the entire eclipse is much longer. Estimates of the dimensions of the two components based on the B and U light curves suggest that the primary M supergiant fills its Roche lobe and produces the gas streaming between the two stars.
The 1976-1978 eclipse of VV Cephei
Marmi, S.
1981
Abstract
Photometric and photographic observations of the long-period variable VV Cephei at the time of its eclipse from 1976 to 1978 are reported. The photoelectric standard UBV observations and photographic R(o)I(o) observations reveal the usual semiregular variations and a short-period flickering in U light. Evaluation of the contact times in B and U indicates that the duration of totality is much shorter than predicted, while the entire eclipse is much longer. Estimates of the dimensions of the two components based on the B and U light curves suggest that the primary M supergiant fills its Roche lobe and produces the gas streaming between the two stars.I documenti in IRIS sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.
