It is a B e main sequence star and was discovered by Dean McLaughlin in It would be larger than the HD system HD b has an orbit 9. Its mass is 8 to Its luminosity is unknown. List of Stars Wiki Explore. Wiki Content. Explore Wikis Community Central.
Register Don't have an account? Based on the star's spectral type of M2 comp , VV Cephei's colour and type is red star. Based on the spectral type, we can deduce that the surface temperature of the star is in the order of between below 3,K based on the notes from Harvard University.
To put this in context, the temperature of our Sun is about 5, Kelvin as said by Google. VV Cephei Luminosity Luminosity is the amount of energy that a star pumps out and its relative to the amount that our star, the Sun gives out.
The figure of 11, VV Cephei estimated radius has been calculated as being The Sun's radius is ,km, therefore the star's radius is an estimated ,, If you need the diameter of the star, you just need to multiple the radius by 2.
However with the release of updated Hipparcos files, the radius is now calculated at being round The figure is derived at by using the formula from SDSS rather than peer reviewed papers. It has been known to produce widely incorrect figures. VV Cephei Iron Abundance is 0. The value comes from the Hipparcos Extended Catalog. VV Cephei apparent magnitude is 5.
Apparent Magnitude is also known as Visual Magnitude. If you used the Parallax value, VV Cephei absolute magnitude is Absolute Magnitude is the apparent magnitude of the star from a distance of 10 parsecs or This assumes that there is nothing in between the object and the viewer such as dust clouds. To really compare the brightness of the star, it is best to use Absolute rather than Apparent Magnitude.
Our own Sun is the brightest star and therefore has the lowest of all magnitudes, A faint star will have a high number. Using the original Hipparcos data that was released in , the parallax to the star was given as 0.
If you want that in miles, it is about 49,,,,, In , Hipparcos data was revised with a new parallax of 1. It should not be taken as though the star is moving closer or further away from Earth. The two stars orbit each other with a period of 7, The supergiant dominates the visual and infrared wavelengths and the companion is more prominent in the ultraviolet part of the spectrum.
The distance has been estimated by a variety of techniques to be around 1. Even though its exact size is uncertain, the red supergiant is believed to have a radius between 1, and 1, times that of the Sun. Some older studies found a larger distance and consequently very high luminosity and radius, but it now seems that the distance is more likely to be around 1.
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