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VV Cephei, also known as HD 208816, is an eclipsing binary star system located in the constellation Cepheus. It is both a B[e] star and shell star. VV Cephei is an eclipsing binary with the third longest known period. A red supergiant fills its Roche lobe when closest to a companion blue star, the latter appearing to be on the main sequence ...
LHires III spectrum of VV Cep observed in the red spectral region out of eclipse, with its central self-absorption feature dividing the observed Hα emission profile into characteristic blue and red components. For each spectrum, the total Hα equivalent width (EW), the EW and peak flux of the blue
Since 2015, an international group of amateurs has informally cooperated using low-resolution spectroscopy (resolving power R = 500–1,000 at Hα wavelength) to observe the 2017–’19 primary eclipse of VV Cep. By maintaining regular observations, it has been possible to show for the first time how low-resolution spectra obtained by amateur ...
25 Νοε 2014 · VV Cephei (M2 Iab + B0–2 V) is the only known ζ Aur binary that has an M-type supergiant. Studies of its atmospheric eclipses provide a valuable extension to what can be learned by eclipse mapping, but are fraught with many challenges.
VV Cephei is a binary star consisting of an M-type supergiant star and a B-type companion on an orbit of 20.36 years. A lot of amateur and professional astronomers as well did contribute particularly during the eclipse 2017-2019 with high professional spectra of the Hα region.
A campaign is planned for the next eclipse of VV Cephei. This paper will provide information on VV Cephei, explain the campaign goals and provide an invitation to observers to do photometry and/or spectroscopy.
VV Cep is an exceptional and unequaled sample of an eclipsing stellar system with a mass exchange between its components during the periastron, in which the blown up bright M2-supergiant with an extended atmosphere is circled by a much weaker hot blue-white main sequence star of spectral class B0Ve...
