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Red supergiants have masses between about 10 M ☉ and 30 or 40 M ☉. [10] Main-sequence stars more massive than about 40 M ☉ do not expand and cool to become red supergiants. Red supergiants at the upper end of the possible mass and luminosity range are the largest known.
Estimated by measuring the fraction of red supergiants at higher luminosities in a large sample of stars. Assumes an effective temperature of 3,625 K. Reported for reference: Theoretical limit of star size (Triangulum Galaxy) ≳1,500 [9] L/T eff: Estimated by measuring the fraction of red supergiants at higher luminosities in a large sample of ...
This is a list of the nearest supergiant stars to Earth, located at a distance of up to 1,100 light-years (340 parsecs) from Earth. Some of the brightest stars in the night sky, such as Rigel and Antares, are in the list.
Supergiants occur in every spectral class from young blue class O supergiants to highly evolved red class M supergiants. Because they are enlarged compared to main-sequence and giant stars of the same spectral type, they have lower surface gravities, and changes can be observed in their line profiles.
Red giants include stars in a number of distinct evolutionary phases of their lives: a main red-giant branch (RGB); a red horizontal branch or red clump; the asymptotic giant branch (AGB), although AGB stars are often large enough and luminous enough to get classified as supergiants; and sometimes other large cool stars such as immediate post ...
A very luminous red supergiant, Mu Cephei is among the largest stars visible to the naked eye, and one of the largest known cool supergiants. It is a runaway star with a peculiar velocity of 80.7 ± 17.7 km/s, [16] and has been described as a hypergiant. [4]
800-290-4726 more ways to reach us. Sign in. Mail. 24/7 Help. For premium support please call: 800-290-4726 more ways to reach us. ... It is a type of massive star called a red supergiant.
VY Canis Majoris is a candidate for a star in a second red supergiant phase, but this is mostly speculative and unconfirmed. [66] From this star CO emission is coincident with the bright KI shell in its asymmetric nebula. The star will produce either: a moderately luminous and long-lasting type IIn supernova (SN IIn) a hypernova; or a