List of largest stars

Below is an ordered list of the largest stars currently known by radius. The unit of measurement used is the radius of the Sun (approximately 695,700 km; 432,288 mi).
The exact order of this list remains very incomplete, as there currently remains great uncertainties especially when deriving various important parameters used in calculations, such as stellar luminosity and effective temperature. Often stellar radii can only be expressed as an average or within a large range of values. Values for stellar radii do vary significantly in sources and throughout the literature, mostly as the boundary of the very tenuous atmosphere (opacity) greatly differs depending on the wavelength of light in which the star is observed.
Several stars can have their radii directly obtained by stellar interferometry. Other methods can use lunar occultations or from eclipsing binaries, which can be used to test other indirect methods of determining true stellar size. Only a few useful supergiant stars can experience occultations by the Moon, including Antares and Aldebaran. Examples of eclipsing binaries include Epsilon Aurigae, VV Cephei, HR 5171, and the red-giant binary system KIC 9246715 in the constellation of Cygnus.[1]
Caveats[edit]

Complex issues exist in determining the true radii of the largest stars, which in many cases do display significant errors. The following lists are generally based on various considerations or assumptions that include:
- Largest stars are usually expressed in units of the solar radius (R☉), where 1.00 R☉ equals 695,700 kilometres.
- Stellar radii or diameters are usually only approximated using Stefan–Boltzmann law for the deduced stellar luminosity and effective surface temperature;
- Stellar distances, and their errors, for most, remain uncertain or poorly determined;
- Many supergiant stars have extended atmospheres and many are embedded within opaque dust shells, making their true effective temperatures highly uncertain;
- Many extended supergiant atmospheres also significantly change in size over time, regularly or irregularly pulsating over several months or years as variable stars. This makes adopted luminosities poorly known and may significantly change the quoted radii;
- Other direct methods for determining stellar radii, rely on lunar occultations or from eclipses in binary systems. This is only possible for a very small number of stars;
- Based on various theoretical evolutionary models, few stars will exceed 1,500–2,000 times the Sun (roughly 3,715 K and Mbol = −9). Such limits maybe also depend on the stellar metallicity.[2]
Extragalactic large stars[edit]
Included within this list are some examples of more distant extragalactic stars, which may have slightly different properties and natures than the currently largest known stars in the Milky Way:
- Some red supergiants in the Magellanic Clouds are suspected to have slightly different limiting temperatures and luminosities. Such stars may exceed accepted limits by undergoing large eruptions or change their spectral types over just a few months. Humphreys et al., for example, calculates the maximum size for a Magellanic cloud star as ~2,600 R☉.[citation needed]
- A survey of the Magellanic Clouds have catalogued many red supergiants, where more than 50 of them exceed 700 R☉ (490,000,000 km; 3.3 AU; 300,000,000 mi). Largest of these is about 1,200-1,300 R☉.[3]
List[edit]
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Method[lower-alpha 1] | Notes |
---|---|---|---|
VY Canis Majoris | 2,069[4][5] (1,420 ± 120)[6][7] |
AD | Used to be described as the largest known star based on a radius of 1,800–2,100 R☉.[8] Older estimates gave the radius of VY CMa as above 3,000 R☉,[9] or as little as 600 R☉.[10] |
LGGS J004539.99+415404.1 | 1,980[11]–2,377[12] | L/Teff | Located in the Andromeda Galaxy |
Orbit of Saturn | 1,940–2,169 | Reported for reference | |
MSX LMC 597 (W60 A27) | 1,882–1,953[13] | L/Teff | Located in the Large Magellanic Cloud |
LGGS J004520.67+414717.3 | 1,870[11]–2,510[12] | L/Teff | Located in the Andromeda Galaxy |
UY Scuti | 1,708 ± 192[14] | AD | This value was based on an angular diameter and distance of 2.9 kpc. Gaia Data Release 2 suggests a distance of 1.55 kpc and a consequently smaller radius of 755 R☉.[15] However, the Gaia parallax is considered unreliable (until further observations) due to a very high level of astrometric noise.[16] |
LGGS J003919.11+404319.2 | 1,685[17] | L/Teff | Located in the Andromeda Galaxy |
WOH S71 (LMC 23095) | 1,662[18]–1,896[19] | L/Teff | Located in the Large Magellanic Cloud |
HV 2242 (WOH S69) | 1,645[19] | L/Teff | Located in the Large Magellanic Cloud |
LGGS J013339.28+303118.8 | 1,565[20]–1,863[12] | L/Teff | Located in the Triangulum Galaxy |
WOH G64 | 1,540 ± 77[21][22] | L/Teff | Located in the Large Magellanic Cloud |
LGGS J013312.26+310053.3 | 1,537[20]–1,765[12] | L/Teff | Located in the Triangulum Galaxy |
MSX LMC 1204 (WOH S72) | 1,537–1,709[13] | L/Teff | Located in the Large Magellanic Cloud |
W61 8-88 (WOH S465) | 1,491[19] | L/Teff | Located in the Large Magellanic Cloud |
HV 888 (WOH S140) | 1,477[23]–1,974[24] | L/Teff | Located in the Large Magellanic Cloud. Another recent estimate gives 1,765 R☉.[19] |
UCAC4 116-007944 (MSX LMC 810) | 1,468[19] | L/Teff | Located in the Large Magellanic Cloud |
W60 A78 (WOH S459) | 1,445[19] | L/Teff | Located in the Large Magellanic Cloud |
HV 12998 (WOH S369) | 1,443[19] | L/Teff | Located in the Large Magellanic Cloud |
W60 A72 (WOH S453) | 1,441[19] | L/Teff | Located in the Large Magellanic Cloud |
WOH S286 | 1,417[19] | L/Teff | Located in the Large Magellanic Cloud |
AH Scorpii | 1,411 ± 124[14] | AD | AH Sco is a variable by nearly 3 magnitudes in the visual range, and an estimated 20% in luminosity. The variation in diameter is not clear because the temperature also varies. |
LGGS J004428.48+415130.9 | 1,410[11]–1,504[12] | L/Teff | Located in the Andromeda Galaxy |
MG73 46 (MSX LMC 891) | 1,385[24]–1,838[19] | L/Teff | Located in the Large Magellanic Cloud |
WOH S281 (IRAS 05261-6614) | 1,376[25]–1,459[19] | L/Teff | Located in the Large Magellanic Cloud |
IRAS 05280-6910 | 1,367[18]–1,738[26] | L/Teff | Located in the Large Magellanic Cloud |
S Persei | 1,364 ± 6[27] | AD | A red supergiant located in the Perseus Double Cluster. Levesque et al. 2005 calculated radii of 780 R☉ and 1,230 R☉ based on K-band measurements.[2] Older estimates gave up to 2,853 R☉ based on higher luminosities.[28] |
PHL 293B | 1,348–1,463[29] | L/Teff | A luminous blue variable star located in the low metallicity galaxy PHL 293B. It is thought to have disappeared. |
LGGS J013414.27+303417.7 | 1,342[20]–1,953[12] | L/Teff | Located in the Triangulum Galaxy |
HV 5993 (WOH S464) | 1,319[24]–1,531[19] | L/Teff | Located in the Large Magellanic Cloud |
SW Cephei | 1,308[30] | AD |
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LGGS J004312.43+413747.1 | 1,270[11]–1,630[12] | L/Teff | Located in the Andromeda Galaxy |
LGGS J004514.91+413735.0 | 1,250[11]–1,575[12] | L/Teff | Located in the Andromeda Galaxy |
LGGS J004428.12+415502.9 | 1,240[11]–1,259[12] | L/Teff | Located in the Andromeda Galaxy |
IRAS 05346-6949 | 1,211[21]–2,064[13] | L/Teff | Located in the Large Magellanic Cloud |
LGGS J004125.23+411208.9 | 1,200[11]–1,602[12] | L/Teff | Located in the Andromeda Galaxy |
HD 90587 | 1,191[30] | AD |
Template:List of largest stars row |
NML Cygni | 1,183[31] | L/Teff | |
LGGS J004524.97+420727.2 | 1,170[11]–1,476[12] | L/Teff | Located in the Andromeda Galaxy |
Westerlund 1-26 | 1,165–1,221[32] | L/Teff | Very uncertain parameters for an unusual star with strong radio emission. The spectrum is variable but apparently the luminosity is not.
Template:List of largest stars row Template:List of largest stars row Template:List of largest stars row |
W60 B90 (WOH S264) | 1,149[25]–2,555[19] | L/Teff | Located in the Large Magellanic Cloud |
HD 62745 | 1,145[30] | AD | |
LGGS J004047.22+404445.5 | 1,140[11]–1,379[12] | L/Teff | Located in the Andromeda Galaxy |
LGGS J004035.08+404522.3 | 1,140[11]–1,354[12] | L/Teff | Located in the Andromeda Galaxy |
MY Cephei | 1,134[33]–2,061[34] | L/Teff | Not to be confused with Mu Cephei (see below). Older estimates have given up to 2,440 R☉ based on much cooler temperatures.[35] |
LGGS J004124.80+411634.7 | 1,130[11]–1,423[12] | L/Teff | Located in the Andromeda Galaxy |
ST Cephei | 1,109[30] | AD |
Template:List of largest stars row |
HD 102115 | 1,100[30] | AD | |
LGGS J004107.11+411635.6 | 1,100[11]–1,207[12] | L/Teff | Located in the Andromeda Galaxy |
LGGS J004031.00+404311.1 | 1,080[11]–1,383[12] | L/Teff | Located in the Andromeda Galaxy
Template:List of largest stars row |
V366 Andromedae | 1,076[30] | AD | |
Trumpler 27-1 | 1,073[15] | L/Teff | Located in the massive possible open cluster Trumpler 27 |
LGGS J004531.13+414825.7 | 1,070[11]–1,420[12] | L/Teff | Located in the Andromeda Galaxy |
IM Cassiopeiae | 1,068[30] | AD |
Template:List of largest stars row |
Orbit of Jupiter | 1,064–1,173 | Reported for reference
Template:List of largest stars row Template:List of largest stars row | |
HR 5171 Aa (V766 Centauri Aa) | 1,060–1,160[36] | L/Teff | |
SU Persei | 1,048[30] | AD |
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LGGS J004114.18+403759.8 | 1,040[11]–1,249[12] | L/Teff | Located in the Andromeda Galaxy |
AS Cephei | 1,026[30] | AD | |
LGGS J004125.72+411212.7 | 1,020[11]–1,359[12] | L/Teff | Located in the Andromeda Galaxy |
LGGS J004059.50+404542.6 | 1,020[11]–1,367[12] | L/Teff | Located in the Andromeda Galaxy |
HD 167861 | 1,016[30] | AD | |
HV 986 (WOH S368) | 1,010[38] | L/Teff | Located in the Large Magellanic Cloud |
The following stars with sizes below 1,000 solar radii are shown for comparison. | |||
CZ Hydrae | 986[39] | L/Teff | One of the coolest stars at 2000 K.[39] |
Mu Cephei (Herschel's "Garnet Star") | 972 ± 228[40] | L/Teff | Prototype of the obsolete class of the Mu Cephei variables and also one of reddest stars in the night sky in terms of the B-V color index.[41] Other estimates have given as high as 1,650 R☉ based on angular diameter.[42] |
V602 Carinae | 932[15]–1,151[30] | AD | |
Betelgeuse (Alpha Orionis) | 764+116 −62[43] |
AD | Star with the third largest apparent size after R Doradus and the Sun. Brightest red supergiant in the night sky. Another estimate gives 955±217 R☉[44] |
Antares A (Alpha Scorpii A) | 707[30] | AD | Antares was originally calculated to be over 850 R☉,[45][46] but those estimates are likely to have been affected by asymmetry of the atmosphere of the star.[47] |
V354 Cephei | 685[15] | L/Teff | |
KY Cygni | 672[15]–1,420[2][48] | L/Teff | |
119 Tauri (CE Tauri) | 587–593[49] | AD | Can be occulted by the Moon, allowing accurate determination of its apparent diameter. |
CW Leonis | 580–686[50] | L/Teff | Prototype of carbon stars. CW Leo was mistakenly identified as the claimed planet "Nibiru" or "Planet X". |
Mira A (Omicron Ceti) | 541[31] | AD | Prototype Mira variable. De beck et al. 2010 calculates 541 R☉.[31] |
VV Cephei A | 516[51]–1,000[52] | EB | VV Cep A is a highly distorted star in a close binary system, losing mass to the secondary for at least part of its orbit. Data from the most recent eclipse has cast additional doubt on the accepted model of the system. Older estimates give up to 1,900 R☉[2] |
V382 Carinae (x Carinae) | 485 ± 40[53] | AD | Yellow hypergiant, one of the rarest types of a star. |
Pistol Star | 435[54] | AD | Blue hypergiant, among the most massive and luminous stars known. |
HD 179821 | 400–450[36] | DSKE | V1427 Aquilae may be a yellow hypergiant or a much less luminous star. |
V509 Cassiopeiae | 390–910[55] | AD | Yellow hypergiant, one of the rarest types of a star. |
Inner limits of the asteroid belt | 380 | Reported for reference | |
IRC +10420 | 380[56] | L/Teff | A yellow hypergiant that has increased its temperature into the LBV range. De beck et al. 2010 calculates 1,342 R☉ based on a much cooler temperature.[31] |
V688 Monocerotis | 372[39] | L/Teff | Also one of the coolest stars at 2000 K.[39] |
R Doradus | 298 ± 21[57] | AD | Star with the second largest apparent size after the Sun. |
Orbit of Mars | 297–358 | Reported for reference | |
La Superba (Y Canum Venaticorum) | 289[30]–352[58] | AD and L/Teff | Referred to as La Superba by Angelo Secchi. Currently one of the coolest and reddest stars. |
Sun's red giant phase | 256[59] | At this point, the Sun will engulf Mercury and Venus, and possibly the Earth although it will move away from its orbit since the Sun will lose a third of its mass. During the helium burning phase, it will shrink to 10 R☉ but will later grow again and become an unstable AGB star, and then a white dwarf after making a planetary nebula.[60][61] Reported for reference | |
Rho Cassiopeiae | 242[30] | AD | Yellow hypergiant, one of the rarest types of a star. |
Eta Carinae A | ~240[62] | Previously thought to be the most massive single star, but in 2005 it was realized to be a binary system. During the Great Eruption, the size was much larger at around 1,400 R☉.[63] η Car is calculated to be between 60 R☉ and 881 R☉.[64] | |
Orbit of Earth | 215 (211–219) | Reported for reference | |
Solar System Habitable Zone | 200–520[65] (uncertain) | Reported for reference | |
Orbit of Venus | 154–157 | Reported for reference | |
Epsilon Aurigae A (Almaaz A) | 143–358[66] | AD | ε Aurigae was incorrectly claimed in 1970 as the largest star with a size between 2,000 R☉ and 3,000 R☉,[67] even though it later turned out not to be an infrared light star but rather a dusk torus surrounding the system. |
Deneb (Alpha Cygni) | 99.84[30] | AD | Prototype Alpha Cygni variable. |
Peony Star | 92[68] | AD | Candidate for most luminous star in the Milky Way. |
Canopus (Alpha Carinae) | 71[69] | AD | Second brightest star in the night sky. |
Orbit of Mercury | 66–100 | Reported for reference | |
LBV 1806-20 | 46–145[70] | L/Teff | Formerly a candidate for the most luminous star in the Milky Way with 40 million L☉,[71] but the luminosity has been revised later only 2 million L☉.[72][73] |
Aldebaran (Alpha Tauri) | 44.13 ± 0.84[74] | AD | Fourteenth brightest star in the night sky |
R136a1 | 39.2[75] | L/Teff | Also on record as one of the most massive and luminous stars known (215 M☉ and 6.2 million L☉). |
Polaris (Alpha Ursae Minoris) | 37.5[76] | AD | The current northern pole star. |
Arcturus (Alpha Boötis) | 24.25[30] | AD | Brightest star in the northern celestial hemisphere. |
HDE 226868 | 20–22[77] | The supergiant companion of black hole Cygnus X-1. The black hole is around 500,000 times smaller than the star. | |
Sun | 1 | The largest object in the Solar System. Reported for reference |
References[edit]
Taken from List of largest stars at Wikipedia, licensed under the Creative Commons Attribution-Sharealike 3.0 Unported License. All authors are listed here.
- ↑ Hełminiak, K.G.; Ukita, N.; Kambe, E.; Konacki, M. (2015). "Absolute Stellar Parameters of KIC 09246715: A Double-giant Eclipsing System with a Solar-like Oscillator". The Astrophysical Journal Letters. 813 (2): L25. arXiv:1509.03340. Bibcode:2015ApJ...813L..25H. doi:10.1088/2041-8205/813/2/L25.
- ↑ 2.0 2.1 2.2 2.3 Table 4 in Levesque, Emily M.; Massey, Philip; Olsen, K. A. G.; Plez, Bertrand; Josselin, Eric; Maeder, Andre; Meynet, Georges (2005). "The Effective Temperature Scale of Galactic Red Supergiants: Cool, but Not as Cool as We Thought". The Astrophysical Journal. 628 (2): 973. arXiv:astro-ph/0504337. Bibcode:2005ApJ...628..973L. doi:10.1086/430901. Cite error: Invalid
<ref>
tag; name "levesqueetal2005" defined multiple times with different content Cite error: Invalid<ref>
tag; name "levesqueetal2005" defined multiple times with different content - ↑ Levesque, Emily M.; Massey, Philip; Olsen, K.A.G.; Plez, Bertrand; Meynet, Georges; Maeder, Andre (2006). "The Effective Temperatures and Physical Properties of Magellanic Cloud Red Supergiants: The Effects of Metallicity". The Astrophysical Journal. 645 (2): 1102. arXiv:astro-ph/0603596. Bibcode:2006ApJ...645.1102L. doi:10.1086/504417. Cite error: Invalid
<ref>
tag; name "mc" defined multiple times with different content Cite error: Invalid<ref>
tag; name "mc" defined multiple times with different content - ↑ Matsuura, Mikako; Yates, J. A.; Barlow, M. J.; Swinyard, B. M.; Royer, P.; Cernicharo, J.; Decin, L.; Wesson, R.; Polehampton, E. T.; Blommaert, J. A. D. L.; Groenewegen, M. A. T. (2013-10-30). "Herschel SPIRE and PACS observations of the red supergiant VY CMa: analysis of the molecular line spectra". Monthly Notices of the Royal Astronomical Society. 437 (1): 532–546. arXiv:1310.2947. doi:10.1093/mnras/stt1906. ISSN 0035-8711. Unknown parameter
|s2cid=
ignored (help) - ↑ Neufeld, David A.; Menten, Karl M.; Durán, Carlos; Güsten, Rolf; Kaufman, Michael J.; Kraus, Alex; Mazumdar, Parichay; Melnick, Gary J.; Ortiz-Leon, Gisela; Wiesemeyer, Helmut; Wyrowski, Friedrich (2020-11-03). "Terahertz Water Masers: II. Further SOFIA/GREAT Detections toward Circumstellar Outflows, and a Multitransition Analysis". arXiv:2011.01807 [astro-ph.GA].
- ↑ Gordon, Michael S.; Jones, Terry J.; Humphreys, Roberta M.; Ertel, Steve; Hinz, Philip M.; Hoffman, William F.; Stone, Jordan; Spalding, Eckhart; Vaz, Amali (February 2019). "Thermal Emission in the Southwest Clump of VY CMa". The Astronomical Journal. 157 (2): 57. arXiv:1811.05998. Bibcode:2019AJ....157...57G. doi:10.3847/1538-3881/aaf5cb. Unknown parameter
|s2cid=
ignored (help) - ↑ Wittkowski, M.; Hauschildt, P. H.; Arroyo-Torres, B.; Marcaide, J. M. (2012). "Fundamental properties and atmospheric structure of the red supergiant VY Canis Majoris based on VLTI/AMBER spectro-interferometry". Astronomy & Astrophysics. 540: L12. arXiv:1203.5194. Bibcode:2012A&A...540L..12W. doi:10.1051/0004-6361/201219126. Unknown parameter
|s2cid=
ignored (help) - ↑ Humphreys, Roberta M. (2006). "VY Canis Majoris: The Astrophysical Basis of Its Luminosity". pp. astro–ph/0610433. arXiv:astro-ph/0610433.
- ↑ Monnier, J. D; Millan-Gabet, R; Tuthill, P. G; Traub, W. A; Carleton, N. P; Coudé Du Foresto, V; Danchi, W. C; Lacasse, M. G; Morel, S; Perrin, G; Porro, I. L; Schloerb, F. P; Townes, C. H (2004). "High-Resolution Imaging of Dust Shells by Using Keck Aperture Masking and the IOTA Interferometer". The Astrophysical Journal. 605 (1): 436–461. arXiv:astro-ph/0401363. Bibcode:2004ApJ...605..436M. doi:10.1086/382218. Unknown parameter
|s2cid=
ignored (help) - ↑ Massey, Philip; Levesque, Emily M.; Plez, Bertrand (August 2006). "Bringing VY Canis Majoris Down to Size: An Improved Determination of Its Effective Temperature". The Astrophysical Journal. 646 (2): 1203–1208. arXiv:astro-ph/0604253. Bibcode:2006ApJ...646.1203M. doi:10.1086/505025. Unknown parameter
|s2cid=
ignored (help) - ↑ 11.00 11.01 11.02 11.03 11.04 11.05 11.06 11.07 11.08 11.09 11.10 11.11 11.12 11.13 11.14 11.15 11.16 Massey, Philip; Evans, Kate Anne (2016). "The Red Supergiant Content of M31". The Astrophysical Journal. 826 (2): 224. arXiv:1605.07900. Bibcode:2016ApJ...826..224M. doi:10.3847/0004-637X/826/2/224. Unknown parameter
|s2cid=
ignored (help) - ↑ 12.00 12.01 12.02 12.03 12.04 12.05 12.06 12.07 12.08 12.09 12.10 12.11 12.12 12.13 12.14 12.15 12.16 12.17 12.18 12.19 Gordon, Michael S.; Humphreys, Roberta M.; Jones, Terry J. (July 2016). "Luminous and Variable Stars in M31 and M33. III. The Yellow and Red Supergiants and Post-red Supergiant Evolution". The Astrophysical Journal. 825 (1): 50. arXiv:1603.08003. Bibcode:2016ApJ...825...50G. doi:10.3847/0004-637X/825/1/50. ISSN 0004-637X. Unknown parameter
|s2cid=
ignored (help) - ↑ 13.0 13.1 13.2 Jones, O. C.; Woods, P. M.; Kemper, F.; Kraemer, K. E.; Sloan, G. C.; Srinivasan, S.; Oliveira, J. M.; van Loon, J. Th.; Boyer, M. L.; Sargent, B. A.; McDonald, I.; Meixner, M.; Zijlstra, A. A.; Ruffle, P. M. E.; Lagadec, E.; Pauly, T.; Sewiło, M.; Clayton, G. C.; Volk, K. (2017-05-08). "The SAGE-Spec Spitzer Legacy program: the life-cycle of dust and gas in the Large Magellanic Cloud. Point source classification – III". Monthly Notices of the Royal Astronomical Society. 470 (3): 3250–3282. arXiv:1705.02709. Bibcode:2017MNRAS.470.3250J. doi:10.1093/mnras/stx1101. Unknown parameter
|s2cid=
ignored (help) - ↑ 14.0 14.1 Arroyo-Torres, B.; Wittkowski, M.; Marcaide, J. M.; Hauschildt, P. H. (6 June 2013). "The atmospheric structure and fundamental parameters of the red supergiants AH Scorpii, UY Scuti, and KW Sagittarii". Astronomy & Astrophysics. 554: A76. arXiv:1305.6179. Bibcode:2013A&A...554A..76A. doi:10.1051/0004-6361/201220920.
- ↑ 15.0 15.1 15.2 15.3 15.4 Messineo, M.; Brown, A. G. A. (2019). "A Catalog of Known Galactic K-M Stars of Class I Candidate Red Supergiants in Gaia DR2". The Astronomical Journal. 158 (1): 20. arXiv:1905.03744. Bibcode:2019AJ....158...20M. doi:10.3847/1538-3881/ab1cbd. Unknown parameter
|s2cid=
ignored (help) - ↑ Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
- ↑ Massey, Philip; Kathryn F., Neugent; Levesque, Emily M.; Drout, Maria R.; Courteau, Stéphane (February 2021). "The Red Supergiant Content of M31 and M33". arXiv:2011.13279. Bibcode:2021AJ....161...79M.
- ↑ 18.0 18.1 Steven R. Goldman; Jacco Th. van Loon (2016). "The wind speeds, dust content, and mass-loss rates of evolved AGB and RSG stars at varying metallicity". Monthly Notices of the Royal Astronomical Society. 465 (1): 403–433. arXiv:1610.05761. Bibcode:2017MNRAS.465..403G. doi:10.1093/mnras/stw2708. Unknown parameter
|s2cid=
ignored (help) - ↑ 19.00 19.01 19.02 19.03 19.04 19.05 19.06 19.07 19.08 19.09 19.10 19.11 19.12 Ren, Yi; Jiang, Bi-Wei (2020-07-20). "On the Granulation and Irregular Variation of Red Supergiants". The Astrophysical Journal. 898 (1): 24. arXiv:2006.06605. Bibcode:2020ApJ...898...24R. doi:10.3847/1538-4357/ab9c17. ISSN 1538-4357.
- ↑ 20.0 20.1 20.2 Maria R. Drout; Philip Massey; Georges Meynet (2012). "The yellow and red supergiants of M33". The Astrophysical Journal. 750 (2): 97. arXiv:1203.0247. Bibcode:2012ApJ...750...97D. doi:10.1088/0004-637X/750/2/97. Unknown parameter
|s2cid=
ignored (help) - ↑ 21.0 21.1 University, Keele (December 2017). Research, Keele University (doctoral thesis). Keele University.
- ↑ Levesque, E. M.; Massey, P.; Plez, B.; Olsen, K. A. G. (2009). "The Physical Properties of the Red Supergiant WOH G64: The Largest Star Known?". The Astronomical Journal. 137 (6): 4744. arXiv:0903.2260. Bibcode:2009AJ....137.4744L. doi:10.1088/0004-6256/137/6/4744. Unknown parameter
|s2cid=
ignored (help) - ↑ Kamath, D.; Wood, P. R.; Van Winckel, H. (December 2015). "Optically visible post-AGB stars, post-RGB stars and young stellar objects in the Large Magellanic Cloud". Monthly Notices of the Royal Astronomical Society. 454 (2): 1468–1502. arXiv:1508.00670. Bibcode:2015MNRAS.454.1468K. doi:10.1093/mnras/stv1202. Unknown parameter
|s2cid=
ignored (help) - ↑ 24.0 24.1 24.2 Groenewegen, M. A. T.; Sloan, G. C. (2018). "Luminosities and mass-loss rates of Local Group AGB stars and red supergiants". Astronomy & Astrophysics. 609: A114. arXiv:1711.07803. Bibcode:2018A&A...609A.114G. doi:10.1051/0004-6361/201731089. Unknown parameter
|s2cid=
ignored (help) - ↑ 25.0 25.1 Groenewegen, Martin A. T.; Sloan, Greg C. (January 2018). "Luminosities and mass-loss rates of Local Group AGB stars and Red Supergiants". Astronomy & Astrophysics. 609: A114. arXiv:1711.07803. Bibcode:2018A&A...609A.114G. doi:10.1051/0004-6361/201731089. ISSN 0004-6361.
- ↑ Matsuura, Mikako; Sargent, B.; Swinyard, Bruce; Yates, Jeremy; Royer, P.; Barlow, M. J.; Boyer, Martha; Decin, L.; Khouri, Theo; Meixner, Margaret; Van Loon, Jacco Th.; Woods, Paul M. (2016). "The mass-loss rates of red supergiants at low metallicity: Detection of rotational CO emission from two red supergiants in the Large Magellanic Cloud". Monthly Notices of the Royal Astronomical Society. 462 (3): 2995. arXiv:1608.01729. Bibcode:2016MNRAS.462.2995M. doi:10.1093/mnras/stw1853. Unknown parameter
|s2cid=
ignored (help) - ↑ Norris, Ryan P. (2019). Seeing Stars Like Never Before: A Long-term Interferometric Imaging Survey of Red Supergiants (PDF) (PhD). Georgia State University.
- ↑ De Jager, C; Nieuwenhuijzen, H; Van Der Hucht, K. A (1988). "Mass loss rates in the Hertzsprung-Russell diagram". Astronomy and Astrophysics Supplement Series. 72: 259. Bibcode:1988A&AS...72..259D. ISSN 0365-0138.
- ↑ Allan, Andrew P.; Groh, Jose H.; Mehner, Andrea; Smith, Nathan; Boian, Ioana; Farrell, Eoin J.; Andrews, Jennifer E. (2020). "The possible disappearance of a massive star in the low-metallicity galaxy PHL 293B". Monthly Notices of the Royal Astronomical Society. 496 (2): 1902. arXiv:2003.02242. Bibcode:2020MNRAS.496.1902A. doi:10.1093/mnras/staa1629. Unknown parameter
|s2cid=
ignored (help) - ↑ 30.00 30.01 30.02 30.03 30.04 30.05 30.06 30.07 30.08 30.09 30.10 30.11 30.12 30.13 30.14 30.15 Cruzalèbes, P.; Petrov, R. G.; Robbe-Dubois, S.; Varga, J.; Burtscher, L.; Allouche, F.; Berio, P.; Hofmann, K. H.; Hron, J.; Jaffe, W.; Lagarde, S.; Lopez, B.; Matter, A.; Meilland, A.; Meisenheimer, K.; Millour, F.; Schertl, D. (2019). "A catalogue of stellar diameters and fluxes for mid-infrared interferometry". Monthly Notices of the Royal Astronomical Society. 490 (3): 3158–3176. arXiv:1910.00542. Bibcode:2019MNRAS.490.3158C. doi:10.1093/mnras/stz2803. Unknown parameter
|s2cid=
ignored (help) - ↑ 31.0 31.1 31.2 31.3 De Beck, E.; Decin, L.; De Koter, A.; Justtanont, K.; Verhoelst, T.; Kemper, F.; Menten, K. M. (2010). "Probing the mass-loss history of AGB and red supergiant stars from CO rotational line profiles. II. CO line survey of evolved stars: Derivation of mass-loss rate formulae". Astronomy and Astrophysics. 523: A18. arXiv:1008.1083. Bibcode:2010A&A...523A..18D. doi:10.1051/0004-6361/200913771. Unknown parameter
|s2cid=
ignored (help) - ↑ Arévalo, Aura (2019). The Red Supergiants in the Supermassive Stellar Cluster Westerlund 1 (Thesis). doi:10.11606/D.14.2019.tde-12092018-161841.
- ↑ Beasor, Emma R; Davies, Ben; Arroyo-Torres, B; Chiavassa, A; Guirado, J. C; Marcaide, J. M; Alberdi, A; De Wit, W. J; Hofmann, K. -H; Meilland, A; Millour, F; Mohamed, S; Sanchez-Bermudez, J (2018). "The evolution of red supergiant mass-loss rates". Monthly Notices of the Royal Astronomical Society. 475 (1): 55. arXiv:1712.01852. Bibcode:2018MNRAS.475...55B. doi:10.1093/mnras/stx3174. Unknown parameter
|s2cid=
ignored (help) - ↑ Humphreys, Roberta M.; Helmel, Greta; Jones, Terry J.; Gordon, Michael S. (August 2020). "Exploring the Mass Loss Histories of the Red Supergiants". The Astronomical Journal. 160 (3): 145. arXiv:2008.01108. Bibcode:2020AJ....160..145H. doi:10.3847/1538-3881/abab15. Unknown parameter
|s2cid=
ignored (help) - ↑ Fawley, W. M; Cohen, M (1974). "The open cluster NGC 7419 and its M7 supergiant IRC +60375". Astrophysical Journal. 193: 367. Bibcode:1974ApJ...193..367F. doi:10.1086/153171.
- ↑ 36.0 36.1 van Genderen, A. M.; Lobel, A.; Nieuwenhuijzen, H.; Henry, G. W.; De Jager, C.; Blown, E.; Di Scala, G.; Van Ballegoij, E. J. (2019). "Pulsations, eruptions, and evolution of four yellow hypergiants". Astronomy and Astrophysics. 631: A48. arXiv:1910.02460. Bibcode:2019A&A...631A..48V. doi:10.1051/0004-6361/201834358. Unknown parameter
|s2cid=
ignored (help) - ↑ McDonald, I.; Zijlstra, A. A.; Boyer, M. L. (2012). "Fundamental Parameters and Infrared Excesses of Hipparcos Stars". Monthly Notices of the Royal Astronomical Society. 427 (1): 343–57. arXiv:1208.2037. Bibcode:2012MNRAS.427..343M. doi:10.1111/j.1365-2966.2012.21873.x. Unknown parameter
|s2cid=
ignored (help) - ↑ Levesque, Emily M.; Massey, Philip; Olsen, K. A. G.; Plez, Bertrand (20 September 2007). "Late‐Type Red Supergiants: Too Cool for the Magellanic Clouds?". The Astrophysical Journal. 667 (1): 202–212. arXiv:0705.3431. Bibcode:2007ApJ...667..202L. doi:10.1086/520797.
- ↑ 39.0 39.1 39.2 39.3 Siderud, Emelie (2020). Dust emission modelling of AGB stars. Search this book on
- ↑ Montargès, M.; Homan, W.; Keller, D.; Clementel, N.; Shetye, S.; Decin, L.; Harper, G. M.; Royer, P.; Winters, J. M.; Le Bertre, T.; Richards, A. M. S. (2019). "NOEMA maps the CO J = 2 − 1 environment of the red supergiant μ Cep". Monthly Notices of the Royal Astronomical Society. 485 (2): 2417–2430. arXiv:1903.07129. Bibcode:2019MNRAS.485.2417M. doi:10.1093/mnras/stz397. Unknown parameter
|s2cid=
ignored (help) - ↑ Ahad, Abdul (May 1, 2004). "The second 'Garnet Star' after Mu Cephei must be 119 Tauri!". Google Groups. Archived from the original on January 30, 2018. Retrieved January 30, 2018. Unknown parameter
|url-status=
ignored (help) - ↑ "Jim Kaler-Garnet star".
- ↑ Joyce, Meridith; Leung, Shing-Chi; Molnár, László; Ireland, Michael; Kobayashi, Chiaki; Nomoto, Ken'Ichi (2020). "Standing on the Shoulders of Giants: New Mass and Distance Estimates for Betelgeuse through Combined Evolutionary, Asteroseismic, and Hydrodynamic Simulations with MESA". The Astrophysical Journal. 902 (1): 63. arXiv:2006.09837. Bibcode:2020ApJ...902...63J. doi:10.3847/1538-4357/abb8db. Unknown parameter
|s2cid=
ignored (help) - ↑ Neilson, H. R.; Lester, J. B.; Haubois, X. (December 2011). "Weighing Betelgeuse: Measuring the Mass of α Orionis from Stellar Limb-darkening". Astronomical Society of the Pacific. 9th Pacific Rim Conference on Stellar Astrophysics. Proceedings of a conference held at Lijiang, China in 14–20 April 2011. ASP Conference Series, Vol. 451: 117. arXiv:1109.4562. Bibcode:2010ASPC..425..103L.
- ↑ Pugh, T.; Gray, D. F. (2013-02-01). "On the Six-year Period in the Radial Velocity of Antares A". The Astronomical Journal. 145 (2): 38. Bibcode:2013AJ....145...38P. doi:10.1088/0004-6256/145/2/38. ISSN 0004-6256.
- ↑ Baade, R.; Reimers, D. (2007-10-01). "Multi-component absorption lines in the HST spectra of alpha Scorpii B". Astronomy and Astrophysics. 474 (1): 229–237. Bibcode:2007A&A...474..229B. doi:10.1051/0004-6361:20077308. ISSN 0004-6361.
- ↑ Ohnaka, K.; Hofmann, K.-H.; Schertl, D.; Weigelt, G.; Baffa, C.; Chelli, A.; Petrov, R.; Robbe-Dubois, S. (2013). "High spectral resolution imaging of the dynamical atmosphere of the red supergiant Antares in the CO first overtone lines with VLTI/AMBER". Astronomy & Astrophysics. 555: A24. arXiv:1304.4800. Bibcode:2013A&A...555A..24O. doi:10.1051/0004-6361/201321063. Unknown parameter
|s2cid=
ignored (help) - ↑ Dorn-Wallenstein, Trevor Z.; Levesque, Emily M.; Neugent, Kathryn F.; Davenport, James R. A.; Morris, Brett M.; Gootkin, Keyan (2020). "Short Term Variability of Evolved Massive Stars with TESS II: A New Class of Cool, Pulsating Supergiants". The Astrophysical Journal. 902 (1): 24. arXiv:2008.11723. Bibcode:2020ApJ...902...24D. doi:10.3847/1538-4357/abb318. Unknown parameter
|s2cid=
ignored (help) - ↑ Montargès, M.; Norris, R.; Chiavassa, A.; Tessore, B.; Lèbre, A.; Baron, F. (June 2018). "The convective photosphere of the red supergiant CE Tau. I. VLTI/PIONIER H-band interferometric imaging". Astronomy & Astrophysics. 614 (12): A12. arXiv:1802.06086. Bibcode:2018A&A...614A..12M. doi:10.1051/0004-6361/201731471. Unknown parameter
|s2cid=
ignored (help) - ↑ Schmidt, M. R.; He, J. H.; Szczerba, R.; Bujarrabal, V.; Alcolea, J.; Cernicharo, J.; Decin, L.; Justtanont, K.; Teyssier, D.; Menten, K. M.; Neufeld, D. A.; Olofsson, H.; Planesas, P.; Marston, A. P.; Sobolev, A. M.; De Koter, A.; Schöier, F. L. (2016). "Herschel/HIFI observations of the circumstellar ammonia lines in IRC+10216". Astronomy & Astrophysics. 592: A131. arXiv:1606.01878. Bibcode:2016A&A...592A.131S. doi:10.1051/0004-6361/201527290. PMC 5217166. PMID 28065983.
- ↑ Stassun K.G.; et al. (October 2019). "The revised TESS Input Catalog and Candidate Target List". The Astronomical Journal. 158 (4): 138. arXiv:1905.10694. Bibcode:2019AJ....158..138S. doi:10.3847/1538-3881/ab3467. Unknown parameter
|s2cid=
ignored (help) - ↑ Pollmann, E.; Bennett, P. D.; Vollmann, W.; Somogyi, P. (July 2018). "Periodic Hα Emission in the Eclipsing Binary VV Cephei". Information Bulletin on Variable Stars. 6249 (6249): 1. Bibcode:2018IBVS.6249....1P. doi:10.22444/IBVS.6249.
- ↑ Groenewegen, M. A. T. (March 2020). "Analysing the spectral energy distributions of Galactic classical Cepheids". Astronomy and Astrophysics. 635: A33. arXiv:2002.02186. Bibcode:2020A&A...635A..33G. doi:10.1051/0004-6361/201937060. Unknown parameter
|s2cid=
ignored (help)CS1 maint: Date and year (link) - ↑ Lau, R. M.; Herter, T. L.; Morris, M. R.; Adams, J. D. (2014). "Nature Versus Nurture: Luminous Blue Variable Nebulae in and Near Massive Stellar Clusters at the Galactic Center". The Astrophysical Journal. 785 (2): 120. arXiv:1403.5298. Bibcode:2014ApJ...785..120L. doi:10.1088/0004-637X/785/2/120. Unknown parameter
|s2cid=
ignored (help) - ↑ Nieuwenhuijzen, H.; De Jager, C.; Kolka, I.; Israelian, G.; Lobel, A.; Zsoldos, E.; Maeder, A.; Meynet, G. (2012). "The hypergiant HR 8752 evolving through the yellow evolutionary void" (PDF). Astronomy & Astrophysics. 546: A105. Bibcode:2012A&A...546A.105N. doi:10.1051/0004-6361/201117166.
- ↑ Wong, K. T.; Menten, K. M.; Kamiński, T.; Wyrowski, F.; Lacy, J. H.; Greathouse, T. K. (2018). "Circumstellar ammonia in oxygen-rich evolved stars". Astronomy & Astrophysics. 612: A48. arXiv:1710.01027. Bibcode:2018A&A...612A..48W. doi:10.1051/0004-6361/201731873. Unknown parameter
|s2cid=
ignored (help) - ↑ Ohnaka, Keiichi; Weigelt, Gerd; Hofmann, Karl-Heinz (2019). "Infrared Interferometric Three-dimensional Diagnosis of the Atmospheric Dynamics of the AGB Star R Dor with VLTI/AMBER". The Astrophysical Journal. 883 (1): 89. arXiv:1908.06997. Bibcode:2019ApJ...883...89O. doi:10.3847/1538-4357/ab3d2a. Unknown parameter
|s2cid=
ignored (help) - ↑ Tram, L. N.; Lesaffre, P.; Cabrit, S.; Nhung, P. T. (2018). "Bow-shock chemistry in the interstellar medium". arXiv:1808.01439 [astro-ph.SR].
- ↑ Rybicki, K. R.; Denis, C. (2001). "On the Final Destiny of the Earth and the Solar System". Icarus. 151 (1): 130–137. Bibcode:2001Icar..151..130R. doi:10.1006/icar.2001.6591.
- ↑ Schröder, K.-P.; Connon Smith, R. (2008). "Distant future of the Sun and Earth revisited". Monthly Notices of the Royal Astronomical Society. 386 (1): 155–163. arXiv:0801.4031. Bibcode:2008MNRAS.386..155S. doi:10.1111/j.1365-2966.2008.13022.x. Unknown parameter
|s2cid=
ignored (help) - ↑ Vassiliadis, E.; Wood, P.R. (1993). "Evolution of low- and intermediate-mass stars to the end of the asymptotic giant branch with mass loss". The Astrophysical Journal. 413: 641. Bibcode:1993ApJ...413..641V. doi:10.1086/173033.
- ↑ Gull, T. R.; Damineli, A. (2010). "JD13 – Eta Carinae in the Context of the Most Massive Stars". Proceedings of the International Astronomical Union. 5: 373–398. arXiv:0910.3158. Bibcode:2010HiA....15..373G. doi:10.1017/S1743921310009890. Unknown parameter
|s2cid=
ignored (help) - ↑ Smith, Nathan (2011). "Explosions triggered by violent binary-star collisions: Application to Eta Carinae and other eruptive transients". Monthly Notices of the Royal Astronomical Society. 415 (3): 2020–2024. arXiv:1010.3770. Bibcode:2011MNRAS.415.2020S. doi:10.1111/j.1365-2966.2011.18607.x. Unknown parameter
|s2cid=
ignored (help) - ↑ D. John Hillier; K. Davidson; K. Ishibashi; T. Gull (June 2001). "On the Nature of the Central Source in η Carinae". Astrophysical Journal. 553 (837): 837. Bibcode:2001ApJ...553..837H. doi:10.1086/320948.
- ↑ Ramirez, Ramses; Kaltenegger, Lisa (2017). "A Volcanic Hydrogen Habitable Zone". The Astrophysical Journal Letters. 837 (1): L4. arXiv:1702.08618. Bibcode:2017ApJ...837L...4R. doi:10.3847/2041-8213/aa60c8. Unknown parameter
|s2cid=
ignored (help) - ↑ Kloppenborg, B.K.; Stencel, R.E.; Monnier, J.D.; Schaefer, G.H.; Baron, F.; Tycner, C.; Zavala, R.T.; Hutter, D.; Zhao, M.; Che, X.; Ten Brummelaar, T.A.; Farrington, C.D.; Parks, R.; McAlister, H. A.; Sturmann, J.; Sturmann, L.; Sallave-Goldfinger, P.J.; Turner, N.; Pedretti, E.; Thureau, N. (2015). "Interferometry of ɛ Aurigae: Characterization of the Asymmetric Eclipsing Disk". The Astrophysical Journal Supplement Series. 220 (1): 14. arXiv:1508.01909. Bibcode:2015ApJS..220...14K. doi:10.1088/0067-0049/220/1/14. Unknown parameter
|s2cid=
ignored (help) - ↑ "Ask Andy: The Biggest Star". Ottawa Citizen. Nov 27, 1970. p. 23.
- ↑ Barniske, A.; Oskinova, L. M.; Hamann, W. -R. (2008). "Two extremely luminous WN stars in the Galactic center with circumstellar emission from dust and gas". Astronomy and Astrophysics. 486 (3): 971. arXiv:0807.2476. Bibcode:2008A&A...486..971B. doi:10.1051/0004-6361:200809568. Unknown parameter
|s2cid=
ignored (help) - ↑ Cruzalebes, P.; Jorissen, A.; Rabbia, Y.; Sacuto, S.; Chiavassa, A.; Pasquato, E.; Plez, B.; Eriksson, K.; Spang, A.; Chesneau, O. (2013). "Fundamental parameters of 16 late-type stars derived from their angular diameter measured with VLTI/AMBER". Monthly Notices of the Royal Astronomical Society. 434 (1): 437–450. arXiv:1306.3288. Bibcode:2013MNRAS.434..437C. doi:10.1093/mnras/stt1037. Unknown parameter
|s2cid=
ignored (help) - ↑ Eikenberry, S. S.; Matthews, K.; Lavine, J. L.; Garske, M. A.; Hu, D.; Jackson, M. A.; Patel, S. G.; Barry, D. J.; Colonno, M. R.; Houck, J. R.; Wilson, J. C.; Corbel, S.; Smith, J. D. (2004). "Infrared Observations of the Candidate LBV 1806‐20 and Nearby Cluster Stars". The Astrophysical Journal. 616 (1): 506–518. arXiv:astro-ph/0404435. Bibcode:2004ApJ...616..506E. doi:10.1086/422180. Unknown parameter
|s2cid=
ignored (help) - ↑ Kennedy, Meghan. "LBV 1806-20 AB?". SolStation.com. Archived from the original on 2017-11-13. Retrieved 2017-10-28. Unknown parameter
|url-status=
ignored (help) - ↑ Figer, D. F.; Najarro, F.; Kudritzki, R. P. (2004). "The Double-lined Spectrum of LBV 1806-20". The Astrophysical Journal. 610 (2): L109–L112. arXiv:astro-ph/0406316. Bibcode:2004ApJ...610L.109F. doi:10.1086/423306. Unknown parameter
|s2cid=
ignored (help) - ↑ Nazé, Y.; Rauw, G.; Hutsemékers, D. (2012). "The first X-ray survey of Galactic luminous blue variables". Astronomy & Astrophysics. 538 (47): A47. arXiv:1111.6375. Bibcode:2012A&A...538A..47N. doi:10.1051/0004-6361/201118040. Unknown parameter
|s2cid=
ignored (help) - ↑ Farr, Will M.; Pope, Benjamin J. S.; Davies, Guy R.; North, Thomas S. H.; White, Timothy R.; Barrett, Jim W.; Miglio, Andrea; Lund, Mikkel N.; Antoci, Victoria; Fredslund Andersen, Mads; Grundahl, Frank; Huber, Daniel (2018). "Aldebaran b's Temperate Past Uncovered in Planet Search Data" (PDF). The Astrophysical Journal. 865 (2): L20. arXiv:1802.09812. Bibcode:2018ApJ...865L..20F. doi:10.3847/2041-8213/aadfde. Archived from the original (PDF) on 2020-03-03. Retrieved 2019-12-16. Unknown parameter
|url-status=
ignored (help); Unknown parameter|s2cid=
ignored (help) - ↑ Bestenlehner, Joachim M.; Crowther, Paul A.; Caballero-Nieves, Saida M.; Schneider, Fabian R. N.; Simón-Díaz, Sergio; Brands, Sarah A.; De Koter, Alex; Gräfener, Götz; Herrero, Artemio; Langer, Norbert; Lennon, Daniel J.; Maíz Apellániz, Jesus; Puls, Joachim; Vink, Jorick S. (2020). "The R136 star cluster dissected with Hubble Space Telescope/STIS. II. Physical properties of the most massive stars in R136". Monthly Notices of the Royal Astronomical Society. 499 (2): 1918. arXiv:2009.05136. Bibcode:2020MNRAS.499.1918B. doi:10.1093/mnras/staa2801. Unknown parameter
|s2cid=
ignored (help) - ↑ Fadeyev, Y. A. (2015). "Evolutionary status of Polaris". Monthly Notices of the Royal Astronomical Society. 449 (1): 1011–1017. arXiv:1502.06463. Bibcode:2015MNRAS.449.1011F. doi:10.1093/mnras/stv412. Unknown parameter
|s2cid=
ignored (help) - ↑ Ziółkowski, J. (2005). "Evolutionary constraints on the masses of the components of HDE 226868/Cyg X-1 binary system". Monthly Notices of the Royal Astronomical Society. 358 (3): 851–859. arXiv:astro-ph/0501102. Bibcode:2005MNRAS.358..851Z. doi:10.1111/j.1365-2966.2005.08796.x. Unknown parameter
|s2cid=
ignored (help) Note: For radius, see Table 1 with d=2 kpc.
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Other articles of the topic Star : Sirius, Rigel, Star
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- Constellation
- Lists of stars
- List of most massive stars
- List of most luminous stars
- List of hottest stars
- List of coolest 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
References[edit]
External links[edit]
- Giant Stars An interactive website comparing the Earth and the Sun to some of the largest known stars
- BBC News Three largest stars identified
- Universe Today What is the Biggest Star in the Universe?
This article "List of largest stars" is from Wikipedia. The list of its authors can be seen in its historical. Articles copied from Draft Namespace on Wikipedia could be seen on the Draft Namespace of Wikipedia and not main one.
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