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It is a type of massive star called a red supergiant. "Its estimated mass means it has lived for about 10 to 20 million years, and will soon die," van Loon said.
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 ...
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
N6946-BH1 is a disappearing supergiant star and failed supernova candidate formerly seen in the galaxy NGC 6946, on the northern border of the constellation of Cygnus.The star, either a red supergiant [1] or a yellow hypergiant, [3] was 25 times the mass of the Sun, and was 20 million light years distant from Earth.
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]
Betelgeuse is a red supergiant that has evolved from an O-type main-sequence star. After core hydrogen exhaustion, Betelgeuse evolved into a blue supergiant before evolving into its current red supergiant form. [173] Its core will eventually collapse, producing a supernova explosion and leaving behind a compact remnant. The details depend on ...
Ascension to red giant or red supergiant status; Some of these causes are discussed below, along with the consequences of such phenomenon. Artist's impression of a massive O-type star 'sucking' the mass of its companion in a binary system, living up to its nickname, 'vampire star'. [1]
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]