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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 ...
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 ...
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]
Many of the well-known bright stars are red giants, because they are luminous and moderately common. The red-giant branch variable star Gamma Crucis is the nearest M-class giant star at 88 light-years. [25] The K1.5 red-giant branch star Arcturus is 36 light-years away. [26]
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 ...
While it is frequently described as a yellow supergiant, especially in evolutionary terms, [2] it is classified as a bright giant based on spectrum. [3] Sargas (θ Scorpii A) 329 ± 9 [5] F0Ib-F1III [6] or F0 II [7] 35.5 × 26.3 [5] 3.1 +0.37 −0.32 [5] 1.862 [8] Either a lower luminosity supergiant or a (bright) giant, formed after stellar ...
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The lack of blue supergiants, particularly in a cluster of just the right size and age to include five red supergiants, is unusual. Such low ratios of blue:red supergiants occur in low metallicity clusters, but NGC 7419 is young and has near-solar metallicity. Rapidly rotating stars may account for this evolutionary trend, encouraging high mass ...