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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 ...
RSGC1 (Red Supergiant Cluster 1) is a young massive open cluster in the Milky Way galaxy. It was discovered in 2006 in the data generated by several infrared surveys, named for the unprecedented number of red supergiant members. [3] The cluster is located in the constellation Scutum at the distance of about 6.6 kpc from the Sun.
UY Scuti is a dust-enshrouded bright red supergiant [16] and is classified as a semiregular variable with an approximate pulsation period of 740 days. [5] [17] [18] Based on an old radius of 1,708 R ☉, this pulsation would be an overtone of the fundamental pulsation period, or it may be a fundamental mode corresponding to a smaller radius. [19]
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.
VY Canis Majoris (abbreviated to VY CMa) is an extreme oxygen-rich red hypergiant or red supergiant (O-rich RHG or RSG) and pulsating variable star 1.2 kiloparsecs (3,900 light-years) from the Solar System in the slightly southern constellation of Canis Major.
AH Scorpii is a dust-enshrouded red supergiant [10] and is classified as a semiregular variable star with a main period of 714 days. The total visual magnitude range is 6.5 - 9.6. [ 2 ] No long secondary periods have been detected. [ 11 ]
Colour-Magnitude Diagram showing evolutionary tracks for stars in the super-AGB mass range. A super-AGB star is a star with a mass intermediate between those that end their lives as a white dwarf and those that end with a core collapse supernova, and properties intermediate between asymptotic giant branch (AGB) stars and red supergiants.
Post-red supergiant stars have a generally higher level of nitrogen relative to carbon due to convection of CNO-processed material to the surface and the complete loss of the outer layers. Surface enhancement of helium is also stronger in post-red supergiants, representing more than a third of the atmosphere. [28] [29]