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Betelgeuse

HIP 27989; Alpha Ori; 58 Ori

Estrela Variável Observável Excelente (61/100)

Range: 0.0 - 1.6, Period: 420.0d, Type: SRC

HIP 27989; Alpha Ori; 58 Ori VariableStar Ori Visível Nível 1 Naked eye / Binoculars - Monitor brightness changes
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Propriedades Físicas

Magnitude 0.50
Intervalo 0.0 - 1.6
Período 420.000 dias
Tipo de Variável Semi-Regular Variable (Supergiant)
Tipo Espectral M4Ib
Cor da Estrela Vermelho (B-V 1.85)
Temperatura 3479 K
Raio 887.0 R☉
Distância 488.6 ly

Posição e Identificadores

RA 05h 55m 10.3s
Dec +07° 24' 25.0"
Constelação Ori
HR 2061
HIP 27989
Bayer Alpha
Flamsteed 58 Ori
Variable ID Alp Ori
Double Cat 4506

Visibilidade

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Curva de Luz

Estrelas de Comparação

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Sistema Estelar Múltiplo

Componentes 6
IDs dos Componentes AE
Separação 37.5″
Mag da Companheira 14.5
Ângulo de Posição 113°
Cores das Estrelas A: Vermelho
Descobridor H 6 39

Vista pela Ocular

80x Dawes: 1.9″ TFOV: 0.6°
Realista = tamanho angular verdadeiro
N E 113° A (0.5) B (14.5)

Sep: 37.5″ · PA: 113° · N cima, L esquerda

Resolvido · Rayleigh: 2.3″ · Dawes: 1.9″ · Eff: 3.1″

Comparação de Tamanho

Ciclo de vida estelar

Classificação Espectral

Diagrama Hertzsprung-Russell

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Espectro de corpo negro

Espectro de absorção estelar

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Notas Estelares

ADS 4506A, SRc 0.40 - 1.3V, 2335d. Also superimposed waves 200-400d.
Components B-E all 11 to 14.5v at sep. 40" to 174" from A. D 13.5 at 77", optical. Speckle interferometric observations | in 1983 November (Karovska et al. 1986, ApJ, 308, 360) show A to be a triple system with closer companion at 0.06" | (mag. diff. 3.4 at H alpha) and more distant companion at 0.51" (mag. diff. 4.6 at H alpha).
ADS 4506A, 5.781y, K 3.08k/s, V0 +20.33k/s, asini 81.773.
Ultraviolet FeII emission. 5-micron observations indicate carbon monoxide. STRATOSCOPE II observations indicate infrared | H2O bands. UV observations from OAO-2 indicate C and O underabundant. MgII emissions indicate a cooler shell | surrounding the supergiant.
Expanding circumstellar shell, extending at least 29" or about 600 stellar radii. If rate constant, initial potassium | ejection about 2700 years ago. 2.85-cm radio emission indicates mass loss.
BETELGEUSE; Betelguex; Betelgeuze; Beteiguex; Al Mankib.
The first star whose diameter was measured with the interferometer, .047", by Michelson and Pease at Mt. Wilson in 1920.

Imagem de Levantamento

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Sobre Betelgeuse

Descrição

Betelgeuse is a red supergiant of spectral type M1-M2Ia-Iab, one of the largest stars visible to the naked eye. Located about 650 light-years from Earth, it marks the upper left shoulder of Orion. Betelgeuse is roughly 700-1,000 times the diameter of the Sun — if placed at the center of our solar system, its surface would extend beyond the orbit of Jupiter. It is a semiregular variable star, fluctuating between about magnitude 0.0 and 1.6 over periods of roughly 400 days. Its luminosity is about 100,000 times that of the Sun.

Dicas de Observação

Betelgeuse is instantly recognizable as the distinctly red-orange star at Orion's upper left shoulder. Its color contrast with blue-white Rigel at the opposite corner of Orion is one of the most striking sights in the sky. Monitoring Betelgeuse's brightness changes relative to nearby reference stars (Aldebaran, Pollux, Procyon) is an excellent visual variable star project. Best observed from November through March. In late 2019-early 2020, Betelgeuse underwent an unprecedented dimming event that sparked worldwide attention.

História

The name Betelgeuse likely derives from the Arabic 'Yad al-Jawza' meaning 'hand of the central one,' though the precise etymology is debated. It was among the first stars to have its angular diameter measured, by Albert Michelson and Francis Pease using the Mount Wilson 100-inch telescope's interferometer in 1920. Its variable nature was first noted by Sir John Herschel in 1836.

Curiosidades

Betelgeuse will almost certainly explode as a Type II supernova within the next 100,000 years. When it does, it will briefly shine as bright as the full Moon and be visible in daylight. The 'Great Dimming' of 2019-2020 was likely caused by a massive surface eruption that ejected material which condensed into dust, temporarily blocking part of the star's light.