Lista de las estrellas más grandes

A continuación se muestran listas de las estrellas más grandes conocidas en la actualidad, ordenadas por radio y separadas en categorías por galaxia. La unidad de medida utilizada es el radio del Sol (aproximadamente 695.700  km ; 432.300  mi ). ^[1]

El Sol , la órbita de la Tierra , Júpiter y Neptuno , comparados con cuatro estrellas ( Estrella Pistola , Rho Cassiopeiae , Betelgeuse y VY Canis Majoris )

Descripción general

Aunque las supergigantes rojas suelen considerarse las estrellas más grandes, se ha descubierto que otros tipos de estrellas aumentan temporalmente su radio de forma significativa, como durante las erupciones de LBV o las novas rojas luminosas . Las novas rojas luminosas parecen expandirse con extrema rapidez, alcanzando miles o decenas de miles de radios solares en tan solo unos meses, significativamente más grandes que las supergigantes rojas más grandes. ^[2]

Algunos estudios utilizan modelos que predicen que las estrellas supermasivas (SMS) de Población III o Población I de alta acreción en el universo primitivo podrían haber desarrollado "protoestrellas supergigantes rojas". Se cree que estas protoestrellas tienen tasas de acreción mayores que la tasa de contracción, lo que resulta en temperaturas más bajas pero con radios que alcanzan hasta muchas decenas de miles de R _☉ , comparables a algunos de los agujeros negros más grandes conocidos . ^{[3] [4] [5]}

Diámetros angulares

Los diámetros angulares de las estrellas se pueden medir directamente mediante interferometría estelar . Otros métodos pueden utilizar ocultaciones lunares o de sistemas binarios eclipsantes , que pueden emplearse para probar métodos indirectos de búsqueda de radios estelares. Solo unas pocas supergigantes pueden ser ocultadas por la Luna, incluidas Antares y 119 Tauri . Ejemplos de sistemas binarios eclipsantes son Epsilon Aurigae (Almaaz), VV Cephei y V766 Centauri (HR 5171). Las mediciones del diámetro angular pueden ser inconsistentes porque el límite de la atmósfera muy tenue ( opacidad ) difiere según la longitud de onda de la luz en la que se observa la estrella . ^{[ cita requerida ]}

Sigue habiendo incertidumbres con respecto a la composición y el orden de las listas, especialmente cuando se derivan varios parámetros utilizados en los cálculos, como la luminosidad estelar y la temperatura efectiva . A menudo, los radios estelares solo se pueden expresar como un promedio o estar dentro de un amplio rango de valores. Los valores de los radios estelares varían significativamente en diferentes fuentes y para diferentes métodos de observación. ^{[ cita requerida ]}

Todos los tamaños indicados en estas listas tienen imprecisiones y pueden ser cuestionados. Las listas aún están en proceso de elaboración y los parámetros están sujetos a cambios.

Advertencias

Existen varios problemas a la hora de determinar los radios exactos de las estrellas más grandes, que en muchos casos presentan errores significativos. Las siguientes listas se basan generalmente en diversas consideraciones o suposiciones, entre ellas:

• Los radios o diámetros estelares generalmente se derivan solo de manera aproximada utilizando la ley de Stefan-Boltzmann para la luminosidad estelar deducida y la temperatura superficial efectiva .
• Las distancias estelares y sus errores, para la mayoría de las estrellas, siguen siendo inciertos o están mal determinados.
• Muchas atmósferas supergigantes extendidas también cambian significativamente de tamaño con el tiempo, pulsando de manera regular o irregular durante varios meses o años como estrellas variables . Esto hace que las luminosidades adoptadas sean poco conocidas y pueden cambiar significativamente los radios citados.
• Otros métodos directos para determinar los radios estelares se basan en ocultaciones lunares o eclipses en sistemas binarios, lo que sólo es posible para un número muy pequeño de estrellas.
• Muchas estimaciones de distancia para las supergigantes rojas provienen de la pertenencia a cúmulos o asociaciones estelares, porque es difícil calcular distancias precisas para las supergigantes rojas que no forman parte de ningún cúmulo o asociación.
• En estas listas se incluyen algunos ejemplos de estrellas extragalácticas extremadamente distantes, que pueden tener propiedades y naturalezas ligeramente diferentes a las estrellas más grandes conocidas actualmente en la Vía Láctea . Por ejemplo, se sospecha que algunas supergigantes rojas en las Nubes de Magallanes tienen temperaturas y luminosidades límite ligeramente diferentes . Dichas estrellas pueden superar los límites aceptados al experimentar grandes erupciones o cambiar sus tipos espectrales en tan solo unos meses (o potencialmente años). ^{[6] [7]}

Liza

Las siguientes listas muestran las estrellas más grandes conocidas según la galaxia anfitriona.

vía Láctea

Nubes de Magallanes

Galaxias Andrómeda (M31) y Triángulo (M33)

Otras galaxias (dentro del Grupo Local)

Fuera del Grupo Local (dentro del supercúmulo de Virgo)

Outside the Virgo supercluster

Note that this list does not include the candidate JWST dark stars, with estimated radii of up to 61 astronomical units (13,000 R_☉)^[139] or Quasi-stars, with theoretical models suggesting that they could reach radii of up to 40,700 solar radii (189 au).^[140]

Transient events

During some transient events, such as red novae or LBV eruptions the star's radius can increase by a significant amount.

SN Progenitors

Largest stars by apparent size

The following list include the largest stars by their apparent size (angular diameter) as seen from Earth. The unit of measurement is the milliarcsecond (mas), equivalent to 10×10⁻³ arcseconds. Stars with angular diameters larger than 13 milliarcseconds are included.

See also

• Constellation
• Lists of stars
• List of most massive stars
• List of most luminous stars
• List of hottest stars
• List of coolest stars
• List of smallest known stars
• List of most massive black holes
• List of largest nebulae
• List of largest galaxies
• List of largest cosmic structures
• List of largest exoplanets
• List of star extremes
• Star

Notes

1. Methods for calculating the radius:
   • AD: radius calculated from angular diameter and distance
   • L/T_eff: radius calculated from bolometric luminosity and effective temperature
   • SEIS: radius obtained from seismic data
   • OD: radius obtaied from optical depth
2. At the J2000 epoch
3. ^{[9][10][11][12][13]}
4. Using an angular diameter of 7.8±0.64 milliarcseconds^[27] and a distance of 1610+130
   −110 parsecs.^[28]
5. Using an angular diameter of 14.11±0.6 milliarcseconds and a distance of 940+140
   −40 parsecs.
6. Luminosities are calculated using the apparent bolometric magnitude and distances in the following equation:
   10^{0.4 • (4.74−(m_bol+5−5 • log(dist)))}
7. Legend:
   UD=Uniform disk diameter
   LD=Limb-darkened diameter
   Ross=Rosseland diameter
   Est = Estimated using distance and physical radius

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176. Gatewood, George (1 July 2008). "Astrometric Studies of Aldebaran, Arcturus, Vega, the Hyades, and Other Regions". The Astronomical Journal. 136 (1): 452–460. Bibcode:2008AJ....136..452G. doi:10.1088/0004-6256/136/1/452. ISSN 0004-6256.
177. Bailer-Jones, C. A. L.; Rybizki, J.; Fouesneau, M.; Demleitner, M.; Andrae, R. (2021). "Estimating Distances from Parallaxes. V. Geometric and Photogeometric Distances to 1.47 Billion Stars in Gaia Early Data Release 3". The Astronomical Journal. 161 (3): 147. arXiv:2012.05220. Bibcode:2021AJ....161..147B. doi:10.3847/1538-3881/abd806. S2CID 228063812. Data about this star can be seen here.
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179. Richichi, A.; Percheron, I.; Khristoforova, M. (1 February 2005). "CHARM2: An updated Catalog of High Angular Resolution Measurements". Astronomy and Astrophysics. 431 (2): 773–777. Bibcode:2005A&A...431..773R. doi:10.1051/0004-6361:20042039. ISSN 0004-6361.
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181. Min, Cheulhong; Matsumoto, Naoko; Kim, Mi Kyoung; Hirota, Tomoya; Shibata, Katsunori M.; Cho, Se-Hyung; Shizugami, Makoto; Honma, Mareki (1 April 2014). "Accurate Parallax Measurement toward the Symbiotic Star R Aquarii". Publications of the Astronomical Society of Japan. 66 (2): 38. arXiv:1401.5574. doi:10.1093/pasj/psu003. ISSN 2053-051X.
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183. Perrin, G.; Ridgway, S. T.; Verhoelst, T.; Schuller, P. A.; Traub, W. A.; Millan-Gabet, R.; Lacasse, M. G. (1 June 2005). "Study of molecular layers in the atmosphere of the supergiant star μ Cep by interferometry in the K band". Astronomy & Astrophysics. 436 (1): 317–324. arXiv:astro-ph/0502415. Bibcode:2005A&A...436..317P. doi:10.1051/0004-6361:20042313. ISSN 0004-6361.
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External links

• Giant Stars An interactive website comparing the Earth and the Sun to some of the largest known stars
• Three largest stars identified BBC News
• What is the Biggest Star in the Universe? Universe Today