Betelgeuse

Betelgeuse

Location of Betelgeuse (circled)
Observation data Epoch J2000.0      Equinox J2000.0
Constellation	Orion
Pronunciation	/ˈbɛtəldʒuːz, ˈbiːt-, -dʒuːs/ BE(E)T-əl-jooz, -⁠jooss[1][2]
Right ascension	05h 55m 10.30536s[3]
Declination	+07° 24′ 25.4304″[3]
Apparent magnitude (V)	+0.50[4] (0.0–1.6[5])
Characteristics
Evolutionary stage	Red supergiant
Spectral type	M1–M2 Ia–ab[6]
Apparent magnitude (J)	−3.00[7]
Apparent magnitude (K)	−4.05[7]
U−B color index	+2.06[4]
B−V color index	+1.85[4]
Variable type	SRc[8]
Astrometry
Radial velocity (Rv)	+21.91[9] km/s
Proper motion (μ)	RA: 26.42±0.25[10] mas/yr Dec.: 9.60±0.12[10] mas/yr
Parallax (π)	5.95+0.58 −0.85 mas[11]
Distance	408 – 548+90 −49 ly (125[12] – 168.1+27.5 −14.9[11] pc)
Absolute magnitude (MV)	−5.85[13]
Details
Mass	14[12] – 19[11] M☉
Radius	~640[14]–764+116 −62[11] R☉
Luminosity	~65,000[14]–87,100+20,500 −11,200[11] L☉
Surface gravity (log g)	−0.5[15] cgs
Temperature	3,600±200[11] – 3800[12] K
Metallicity [Fe/H]	+0.05[16] dex
Rotation	36±8[17] years
Rotational velocity (v sin i)	5.47±0.25[17] km/s
Age	8.0[18]–14[12] Myr
Other designations
Betelgeuse, α Ori, 58 Ori, HR 2061, BD+7°1055, HD 39801, FK5 224, HIP 27989, SAO 113271, GC 7451, CCDM J05552+0724, AAVSO 0549+07
Database references
SIMBAD	data

Betelgeuse is a red supergiant star in the constellation of Orion. It is usually the tenth-brightest star in the night sky and, after Rigel, the second-brightest in its constellation. It is a distinctly reddish, semiregular variable star whose apparent magnitude, varying between +0.0 and +1.6, has the widest range displayed by any first-magnitude star. Betelgeuse is the brightest star in the night sky at near-infrared wavelengths. Its Bayer designation is α Orionis, Latinised to Alpha Orionis and abbreviated Alpha Ori or α Ori.^[19]

With a radius around 640 times that of the Sun,^[14] if it were at the center of our Solar System, its surface would lie beyond the asteroid belt and it would engulf the orbits of Mercury, Venus, Earth, and Mars. Calculations of Betelgeuse's mass range from slightly under ten to a little over twenty times that of the Sun. For various reasons, its distance has been quite difficult to measure; current best estimates are of the order of 400–600 light-years from the Sun – a comparatively wide uncertainty for a relatively nearby star. Its absolute magnitude is about −6. Less than 10 million years old, Betelgeuse has evolved rapidly because of its large mass and is expected to end its evolution with a supernova explosion, most likely within 100,000 years. When Betelgeuse explodes, it will shine as bright as the half-Moon for more than three months; life on Earth will be unharmed. Having been ejected from its birthplace in the Orion OB1 association – which includes the stars in Orion's Belt – this runaway star has been observed to be moving through the interstellar medium at a speed of 30 km/s, creating a bow shock over four light-years wide.

Betelgeuse became the first extrasolar star whose photosphere's angular size was measured in 1920, and subsequent studies have reported an angular diameter (i.e., apparent size) ranging from 0.042 to 0.056 arcseconds; that range of determinations is ascribed to non-sphericity, limb darkening, pulsations and varying appearance at different wavelengths. It is also surrounded by a complex, asymmetric envelope, roughly 250 times the size of the star, caused by mass loss from the star itself. The Earth-observed angular diameter of Betelgeuse is exceeded only by those of R Doradus and the Sun.

Starting in October 2019, Betelgeuse began to dim noticeably, and by mid-February 2020 its brightness had dropped by a factor of approximately 3, from magnitude 0.5 to 1.7. It then returned to a more normal brightness range, reaching a peak of 0.0 visual and 0.1 V-band magnitude in April 2023. Infrared observations found no significant change in luminosity over the last 50 years, suggesting that the dimming was due to a change in extinction around the star rather than a more fundamental change. A study using the Hubble Space Telescope suggests that occluding dust was created by a surface mass ejection; this material was cast millions of miles from the star, and then cooled to form the dust that caused the dimming.