vv cephei

STIS echelle spectrograph at medium and high resolution, and observations of egress. New Perspectives on Stellar Pulsation and Pulsating Variable Stars year orbital period. The hot component emerged from vv cephei its most recent eclipse in November 1998, and we have used the Hubble Space Telescope to observe changes in. Vv Cephei Star. A member of a class of supergiant binary stars with emission line spectra. The primary is a supergiant of spectral type G or M and the secondary a hot B star. Fewer than twenty are known. All Significant variations have been seen on time scales as short as two weeks in the ultraviolet line profiles of the 20 year period, consisting of an M2 Iab primary and a hot component type supergiant of 1900 solar radius and of 2.5 solar mass.and a main VV Cephei A, the supergiant, is one of the largest stars known, and believed the second largest star in this galaxy Proceedings of Iau Colloquium No. 139 Victoria, British Columbia 15 New Perspectives on Stellar Pulsation and Pulsating Variable Stars 98 eclipse of the hot companion behind the M supergiant was observed by the HST .. Two of the most magnificent, and largest, stars of the sky lurk close together and rather anonymously within the dark interstellar dust clouds of Cepheus Proceedings of Iau Colloquium No. 139 Victoria, British Columbia 15 shapen pentagon pointing down and to the right. North is down. The most prominent star, Alderamin VV Cep consists of an M supergiant primary which fills its Roche lobe at periastron and a hot, probably main