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Rigel, the brightest star in the constellation Orion is a typical blue-white supergiant; the three stars of Orion's Belt are all blue supergiants; Deneb is the brightest star in Cygnus, another blue supergiant; and Delta Cephei (itself the prototype) and Polaris are Cepheid variables and yellow supergiants.
A red supergiant star orbited by a smaller B-type main-sequence star with a radius estimated between 13 [47] and 25 R ☉. [48] Widely recognised as being among the largest known stars. [19] Another estimate give a radius of 660 R ☉ [23] based on the Gaia DR3 distance of 1 kpc. [28] U Lacertae A 1,013 [23] L/T eff: KW Sagittarii: 1,009 ± 142 ...
Some of the brightest stars in the night sky, such as Rigel and Antares, are in the list. While supergiants are typically defined as stars with luminosity classes Ia, Iab or Ib, other definitions exist, such as those based on stellar evolution. [1] Therefore, stars with other luminosity classes can sometimes be considered supergiants.
Mira was historically thought to be a red supergiant star, but is now widely accepted to be an asymptotic giant branch star. [32] Some red supergiants are larger and more luminous, with radii exceeding over a thousand times that of the Sun. These are hence also referred to as red hypergiants: Mu Cephei; VV Cephei A; NML Cygni; S Persei; UY Scuti
Betelgeuse is a red supergiant star in the constellation of Orion. It is usually the tenth-brightest star in the night sky and, after Rigel, the second-brightest in its constellation. It is a distinctly reddish, semiregular variable star whose apparent magnitude, varying between +0.0 and +1.6, has the widest range displayed by any first ...
V762 Cassiopeiae is a red supergiant and a variable star located about 2,500 light-years away in the Cassiopeia constellation. Its apparent magnitude vary between 5.82 and 5.95, which makes it faintly visible to the naked eye under dark skies. It is a relatively cool star with an average surface temperature of 3,869 K.
A star whose initial mass is less than approximately 0.25 M ☉ will not become a giant star at all. For most of their lifetimes, such stars have their interior thoroughly mixed by convection and so they can continue fusing hydrogen for a time in excess of 10 12 years, much longer than the current age of the Universe. They steadily become ...
Stars of greater mass have a higher rate of core energy generation, and heavier stars' luminosities increase far out of proportion to the increase in their masses. The Eddington limit is the point beyond which a star ought to push itself apart, or at least shed enough mass to reduce its internal energy generation to a lower, maintainable rate.