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A probabilistic age prior analysis give a current mass of 16.5–19 M ☉ and an initial mass of 18–21 M ☉. [11] Betelgeuse's mass can also be estimated based on its position on the color‑magnitude‑diagram (CMD). Betelgeuse's color may have changed from yellow (or possibly orange; i.e. a yellow supergiant) to red in the last few ...
For example, if a TNO is incorrectly assumed to have a mass of 3.59 × 10 20 kg based on a radius of 350 km with a density of 2 g/cm 3 but is later discovered to have a radius of only 175 km with a density of 0.5 g/cm 3, its true mass would be only 1.12 × 10 19 kg.
This matches the expected parameters of lower mass red supergiants. A small number of progenitors of type II-L and type IIb supernovae have been observed, all having luminosities around 100,000 L ☉ and somewhat higher temperatures up to 6,000K. These are a good match for slightly higher mass red supergiants with high mass-loss rates.
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−119 [d] or ~R Betelgeuse: L/T eff & AD Widely recognised as being among the largest known stars. [21] Might be the largest star visible to the naked eye. [30] The higher radii estimate assume Mu Cephei is in the Cepheus OB2 OB association. [28] [31] Other sources suggest Mu Cephei and Betelgeuse are likely similar in properties.
Stars fuse (meld together) various elements, depending on their age and mass. By studying movements (like sound waves) on the surface of the star suggest Betelgeuse is still fusing helium.
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