![]() These cool temperatures allow molecules to form in their photospheres and atmospheres. Super-AGB stars occupy the top-right of the Hertzsprung–Russell diagram (HR diagram), and have cool temperatures between 3,000 and 4,000 K, which is similar to normal AGB stars and red supergiant stars (RSG stars). They have initial masses of 7.5–9.25 M ☉ in stellar-evolutionary models, but have exhausted their core hydrogen and helium, left the main sequence, and expanded to become large, cool, and luminous. The combined effect of H-rich envelope collapse and low 12C(α, γ) 16O rate can lead to the formation of BHs with masses consistent with the primary component of GW190521.Stars that have properties between Asymptotic Giant Branch stars and red supergiants Colour-Magnitude Diagram showing evolutionary tracks for stars in the super-AGB mass rangeĪ 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. The onset of this dredge-up is particularly sensitive to the assumed model for convection and mixing. The existence of the mass gap is currently being challenged by the detection of GW190521, with a primary component mass of $85^$, the mass gap is completely removed by the dredge-up effect. Pair-instability (PI) is expected to open a gap in the mass spectrum of black holes (BHs) between ≈40-65 and ≈120 M ⊙.
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