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Below are lists of the largest stars currently known, ordered by radius and separated into categories by galaxy. The unit of measurement used is the radius of the Sun (approximately 695,700 km; 432,300 mi).[1]
Overview
Although red supergiants are often considered the largest stars, some other star types have been found to temporarily increase significantly in radius, such as during LBV eruptions or luminous red novae. Luminous red novae appear to expand extremely rapidly, reaching thousands to tens of thousands of solar radii within only a few months, significantly larger than the largest red supergiants.[2]
Some studies use models that predict high-accreting Population III or Population I supermassive stars (SMSs) in the very early universe could have evolved "red supergiant protostars". These protostars are thought to have accretion rates be larger than the rate of contraction, resulting in lower temperatures but with radii reaching up to many tens of thousands of R☉, comparable to some of the largest known black holes.[3][4][5]
Angular diameters
The angular diameters of stars can be measured directly using stellar interferometry. Other methods can use lunar occultations or from eclipsing binaries, which can be used to test indirect methods of finding stellar radii. Only a few useful supergiant stars can be occulted by the Moon, including Antares A (Alpha Scorpii A). Examples of eclipsing binaries are Epsilon Aurigae (Almaaz), VV Cephei, and V766 Centauri (HR 5171). Angular diameter measurements can be inconsistent because the boundary of the very tenuous atmosphere (opacity) differs depending on the wavelength of light in which the star is observed.
Uncertainties remain with the membership and order of the lists, especially when deriving various parameters used in calculations, such as stellar luminosity and effective temperature. Often stellar radii can only be expressed as an average or be within a large range of values. Values for stellar radii vary significantly in different sources and for different observation methods.
All the sizes stated in these lists have inaccuracies and may be disputed. The lists are still a work in progress and parameters are prone to change.
Caveats
Various issues exist in determining accurate radii of the largest stars, which in many cases do display significant errors. The following lists are generally based on various considerations or assumptions; these include:
- Stellar radii or diameters are usually derived only approximately using the Stefan–Boltzmann law for the deduced stellar luminosity and effective surface temperature.
- Stellar distances, and their errors, for most stars, remain uncertain or poorly determined.
- 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.
- Many distance estimates for red supergiants come from stellar cluster or association membership, because it is difficult to calculate accurate distances for red supergiants that are not part of any cluster or association.
- In these lists are some examples of extremely distant extragalactic stars, which may have slightly different properties and natures than the currently largest known stars in the Milky Way. For example, 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 changing their spectral types over just a few months (or potentially years).[6][7]
Lists
The following lists show the largest known stars based on the host galaxy.
Milky Way
 |
| Star name | Solar radii (Sun = 1) |
Method[a] | Notes |
|---|---|---|---|
| Orbit of Saturn | 2,047–2,049.9[8][b] | Reported for reference | |
| WOH G64 (For comparison) | 1,540[9][10][11][12][13] ± 77[9] | L/Teff | Located in the Large Magellanic Cloud. |
| Theoretical limit of star size (Milky Way) | ~1,500[15] or ~1,800[16] | Lower value comes from the rough average radii of the three largest stars studied in the paper. It is consistent with the largest possible stellar radii predicted from the current evolutionary theory, and it is believed that stars above this radius would be too unstable and usually do not form.[15] Higher value is derived from evolutionary modelling of red supergiants with low metallicites and an initial mass of 50 M☉. Reported for reference | |
| RSGC1-F01 | 1,436,[17] 1,450,[18] 1,530+330 −424[19] |
L/Teff | |
| VY Canis Majoris | 1,420±120[20][21][22] | AD | An extreme oxygen-rich red hypergiant that has experienced two dimming periods in the 20th century where the star became dimmer by up to 2.5 magnitudes.[23] Potentially the largest known star in the Milky Way.[21] |
| AH Scorpii | 1,411±124[24][25] | AD | |
| RSGC1-F06 | 1,382+298 −384[19] |
L/Teff | |
| S Persei | 1,364±6[26] | AD | |
| CD-33 12241 | 1,359[27] | L/Teff | |
| NML Cygni | <1,350+195 −229[c] |
AD | Surrounding dusty region is very complex making the radius hard to determine.[28] |
| Stephenson 2 DFK 2 | 1,301+259 −325[19] |
L/Teff | Another red supergiant, Stephenson 2 DFK 1 has an estimated radius of 2,150 R☉. However, its luminosity is significantly above the Humphreys-Davidson limit and it is potentially not a member of the Stephenson 2 cluster. It also has a distance with an uncertainty of ≳50% due to it only being measured with radial velocities.[19][30] |
| Stephenson 2 DFK 49 | 1,300+258 −323[19] |
L/Teff | A K-type star similar to the yellow hypergiant IRC +10420 that has left its red supergiant stage.[19] |
| CD-26 5055 | 1,280+20 −123[31] |
L/Teff | |
| HD 143183 (V558 Normae) | 1,261[27] | L/Teff | |
| μ Cephei (Herschel's Garnet Star) | 1,259[32][33]–1,420[15][33] | L/Teff | Widely recognised as being among the largest known stars.[34] |
| RSGC1-F10 | 1,246+264 −337[19] |
L/Teff | |
| Westerlund 1 W237 (Westerlund 1 BKS B) | 1,241±70[35] | L/Teff | Possibly a foreground giant.[36] |
| PZ Cassiopeiae | 1,231[27] – 1,364[37] | L/Teff | |
| ST Cephei | 1,218[27] | L/Teff | |
| IRC -10414 | ~1,200[38] | L/Teff | |
| V517 Monocerotis | 1,196+80 −159[31] |
L/Teff | |
| RSGC1-F05 | 1,185+254 −325[19] |
L/Teff | |
| GCIRS 7 | 1,170±60[39]–1,368,[40] 1,359[41] | AD & L/Teff | |
| Westerlund 1 W26 (Westerlund 1 BKS AS) | 1,165±58–1,221±120[35] | L/Teff | |
| EV Carinae | 1,165[42] | L/Teff | |
| 16 | 1,157[27] | L/Teff | |
| WY Velorum A | 1,157[27] | L/Teff | A symbiotic binary.[43] |
| RSGC1-F08 | 1,150+234 −297[19] |
L/Teff | |
| V354 Cephei | 1,139[37] – 1,245[27] | L/Teff | |
| RSGC1-F02 | 1,499,[17] 1,128+238 −303,[19] 1,500[18] |
L/Teff | |
| VX Sagittarii | 1,120 – 1,550,[44] 1,200,[45] 1,356,[46] 1,480[25] | L/Teff | The most luminous known asymptotic giant branch star.[46] Widely recognised as being among the largest known stars.[34] |
| Orbit of Jupiter | 1,114.5–1,115.8[8][b] | Reported for reference | |
| V582 Cassiopeiae | 1,111[27] | L/Teff | |
| RW Cygni | 1,103+251 −177[47] |
AD | |
| RSGC1-F04 | 1,082,[17] 1,100,[18] 1,422+305 −390[19] |
L/Teff | |
| RT Carinae | 1,090±218[15] | L/Teff | |
| V384 Persei | 1,088[48] | L/Teff | |
| UU Persei | 1,079+9 −8[31] |
L/Teff | |
| R Fornacis | 1,078[48] | L/Teff | |
| LL Pegasi | 1,074[49] | L/Teff | |
| HD 126577 | 1,066+9 −32[31] |
L/Teff | |
| V766 Centauri Aa | 1,060–1,160[50] | ? | V766 Centauri Aa is a rare variable yellow hypergiant. |
| V1300 Aquilae (IRC -10529) | 1,059[51] | L/Teff | |
| HaroChavira 1 | 1,058[52] | L/Teff | |
| CM Velorum | 1,048[27] – 1,416.24+0.40 −0.96[31] |
L/Teff | |
| AG Camelopardalis | 1,048[27] | L/Teff | |
| SU Persei | 1,044+31 −21 – 1,139+34 −23[26] |
AD | |
| WX Piscium | 1,044[51] | L/Teff | |
| KU Andromedae (IRC +40004) | 1,044[51] | L/Teff | |
| KY Cygni | 1,032[52] | L/Teff | |
| RSGC1-F11 | 1,032+210 −267[19] |
L/Teff | |
| BC Cygni | 1,031[52]–1,187+34 −37[31] |
L/Teff | A more detailed but older study gives values of 1,081 R☉ (856–1,375) for the year 2000, and 1,303 R☉ (1,021–1,553) for the year 1900.[53] |
| RW Leonis Minoris | 1,028[51] | L/Teff | |
| V346 Puppis | 1,025[48] | L/Teff | |
| V530 Cassiopeiae | 1,017[27] | L/Teff | |
| RSGC1-F13 | 1,017+221 −286,[19] 1,430,[18] 1,097[17] |
L/Teff | |
| V602 Carinae | 1,015[54] | AD | |
| U Lacertae A | 1,013[27] | L/Teff | |
| KW Sagittarii | 1,009±142[24][25] | AD | |
| Ve 4-64 | 1,007[27] | L/Teff | |
| RSGC1-F07 | 1,006+215 −276[19] |
L/Teff | |
| V349 Carinae | 1,002+12 −74[31] |
L/Teff | |
| IRAS 18111-2257 | ~1,000[55] (~8×1013 – 1×1014 cm) | L/Teff | Estimated based on the bolometric luminosity and assumed effective temperature of 2,000 K. Another period-luminosity-derived luminosity for this star results in a radius of 1,730 R☉.[55] |
| V674 Cephei | 999[27] | L/Teff | |
| RSGC1-F09 | 996+210 −269[19] |
L/Teff | |
| CIT 11 | 982[27] | L/Teff | |
| V381 Cephei Aa | 977[27] | L/Teff | |
| MSX6C G086.5890-00.7718 | (975+175 −183–1,035+186 −158)[56]–1,196.91+6.31 −6.35[31] |
L/Teff | Lower values based on the Gaia DR3 effective temperature and the luminosity of Levesque et al. (2005) and that of Messineo & Brown (2019). Higher value based on the GSP Phot-Aeneas library using BR/RP spectra in Gaia DR3. |
| V3953 Sagittarii (IRC -30398) | 970[51] | L/Teff | |
| V396 Centauri | 965[27] | L/Teff | |
| UW Aquilae | 964[27] | L/Teff | |
| S Aurigae | 957[48] | L/Teff |
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