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10 Σεπ 2020 · VV Cephei (M2 Iab + B0.5 V) is the brightest M supergiant in an eclipsing binary system in the sky (V=4.90). Its orbital period of 20.3 years is one of the longest known for an eclipsing binary.
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.
By combining this with measurements of Doppler shifts in the spectral lines, Gaposchkin proposed that the VV Cep system consisted of a 44-solar-mass (M ☉) cool, red supergiant and a 35M ☉ hot blue star – a rare example of a red supergiant binary. The hydrogen emission lines were associated with the hot star and so disappeared during its ...
In this work, we report on a continuing campaign of spectroscopic observations of Hα emission from VV Cep over the period 2015–2020 by amateur observers of the ARAS spectroscopy group. We also present a newly discovered 42-day period variability in the equivalent width of this Hα emission.
3 Οκτ 2018 · We present a high-cadence time series of spectroscopic observations of the Hα emission line profile obtained during the egress and total eclipse phases of the M supergiant binary VV Cephei...
30 Απρ 2006 · 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...
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...
