V391 Pegasi
Star, Stellar Classification, Constellation
978-613-9-12737-5
6139127378
136
2012-01-07
45.00 €
eng
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Please note that the content of this book primarily consists of articles available from Wikipedia or other free sources online. V391 Pegasi, also catalogued as HS 2201+2610, is a blue-white subdwarf star approximately 4,570 light-years away in the constellation of Pegasus. The star is clarified as an "extreme horizontal branch star." It is small with only half the mass and one-over-four-and-one-thirds the diameter of the Sun. It has luminosity 15.4 times the Sun. It could be quite old, perhaps in excess of 10 Gyr. It is a pulsating variable star of the V361 Hydrae type (or also called sdBVr type). Subdwarf B stars such as V391 Pegasi are thought to be the result of the ejection of the hydrogen envelope of a red giant star at or just before the onset of helium fusion. The ejection left only a tiny amount of hydrogen on the surface - less than 1/1000 of the total stellar mass. The future for the star is to eventually cool down to make a low mass white dwarf. Most stars retain more of their hydrogen after the first red giant phase, and eventually become asymptotic giant branch stars. The reasons for why some stars, like V391 Pegasi, lose so much mass are not well known.
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