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Red supergiants develop deep convection zones reaching from the surface over halfway to the core and these cause strong enrichment of nitrogen at the surface, with some enrichment of heavier elements. [26] Some red supergiants undergo blue loops where they temporarily increase in temperature before returning to the red supergiant state. This ...
XX Per is a red supergiant of spectral type M4Ib with an effective temperature below 4,000 K. It has a large infrared excess, indicating surrounding dust at a temperature of 900 K, but no masers have been detected. [14] [15] XX Persei has a mass of 16 solar masses, above the limit beyond which stars end their lives as supernovae. [6]
Red giants vary in the way by which they generate energy: most common red giants are stars on the red-giant branch (RGB) that are still fusing hydrogen into helium in a shell surrounding an inert helium core; red-clump stars in the cool half of the horizontal branch, fusing helium into carbon in their cores via the triple-alpha process
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.
NML Cygni or V1489 Cygni (abbreviated to NML Cyg or V1489 Cyg) is a red hypergiant [4] or red supergiant (RSG) in the constellation Cygnus.It is possibly one of the largest known stars currently known, and is also possibly one of the most luminous and massive cool hypergiants, as well as one of the most luminous stars in the Milky Way.
The most massive red supergiants will evolve back to blue supergiants, Luminous blue variables, or Wolf-Rayet stars before their cores collapse, and Mu Cephei appears to be massive enough for this to happen. A post-red supergiant will produce a type IIn or type II-b supernova, while a Wolf Rayet star will produce a type Ib or Ic supernova. [32]
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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