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Masi is looking forward to collecting scientific observations of the occultation, which acts as a sort of preview for what our night sky will look like one day when Betelgeuse disappears after ...
In late 2019 and early 2020, Betelgeuse blew its top. Literally. Around that time the famous bright star marking the right shoulder of Orion suddenly started dimming, dropping to about half its ...
Found in the constellation Orion, Betelgeuse is extremely bright, especially considering that it’s roughly 650 light-years from Earth (though, it does have a radius 1,000 times bigger than the Sun).
This is what Betelgeuse may have looked like up until about 1 million years ago, when it was a main-sequence star. The surface of Betelgeuse shows enhancement of nitrogen, relatively low levels of carbon, and a high proportion of 13 C relative to 12 C , all indicative of a star that has experienced the first dredge-up .
Betelgeuse, also designated Alpha Orionis, is a massive M-type red supergiant star nearing the end of its life. It is the second brightest star in Orion, and is a semiregular variable star. [7] It serves as the "right shoulder" of the hunter (assuming that he is facing the observer).
Betelgeuse; Epsilon Pegasi; Zeta Cephei; Lambda Velorum; Eta Persei; 31 and 32 Cygni; Psi 1 Aurigae; 119 Tauri; Mira was historically thought to be a red supergiant star, but is now widely accepted to be an asymptotic giant branch star. [32] Some red supergiants are larger and more luminous, with radii exceeding over a thousand times that of ...
By studying movements (like sound waves) on the surface of the star suggest Betelgeuse is still fusing helium. That would mean that the star is not close (on a human timescale) to erupting as a ...
These parameters are all consistent with those estimated for Betelgeuse. [11] The initial mass of Mu Cephei has been estimated from its position relative to theoretical stellar evolutionary tracks to be between 15 M ☉ and 25 M ☉. [11] [15] The star currently has a mass loss rate of (4.9 ± 1.0) × 10 −7 M ☉ per year. [11]