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VV Cephei

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description VV Cephei Overview

VV Cephei is an eclipsing binary system in the constellation Cepheus composed of a very large, cool M-type supergiant and a hotter B-type companion. The two stars orbit each other roughly every 20.3 years, and eclipses last many months because the supergiant has an enormous extended atmosphere. Material from the cool primary interacts with the hot companion, making the system useful for studying mass transfer, stellar winds, and the outer layers of evolved massive stars.

help VV Cephei FAQ

How big is the red supergiant in the VV Cephei system?

The primary star in the VV Cephei system is a red supergiant historically cited as being among the largest known stars, with estimates placing its radius at over 1,000 times that of the Sun. It is so large that if placed in our solar system, it would extend past the orbit of Jupiter.

How long does it take for the two stars in VV Cephei to orbit each other?

The two stars in the VV Cephei binary system have an orbital period of roughly 20 years. Because it is an eclipsing binary, astronomers can observe a significant drop in brightness when the hot blue companion passes behind the massive red supergiant.

Where can I find VV Cephei in the night sky?

VV Cephei is located in the northern constellation of Cepheus. While it is too faint to be seen with the naked eye, amateur astronomers with medium to large telescopes can observe it.

What type of companion star orbits the red supergiant in VV Cephei?

The companion in the VV Cephei system is a hot blue main-sequence star that orbits the massive red supergiant. The interaction between the cooler, swollen red supergiant and the intensely hot blue companion creates complex mass-transfer phenomena between the two bodies.

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