Astronomy:List of largest stars
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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 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
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.[6]
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.[7]
- 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).[8][9]
Lists
The following lists show the largest known stars based on the host galaxy.
Milky Way
| Star name | Solar radius (R☉) | Method[lower-alpha 1] | Notes |
|---|---|---|---|
| Orbit of Saturn | 2,047–2,049.9[10][lower-alpha 2] | Reported for reference | |
| Theoretical limit of star size (Milky Way) | ≳1,700[11] | L/Teff | Estimated by measuring the fraction of red supergiants at higher luminosities in a large sample of supernova progenitor candidates. Assumes an effective temperature of 3,605 K. Reported for reference |
| WOH G64 A (For comparison) | 1,540[12][13][14][15][16] ± 77[12] | L/Teff | Located in the Large Magellanic Cloud. |
| RSGC1-F01 (FMR2006 1) | 1,530+330 −424[18] |
L/Teff | |
| RSGC1-F04 (FMR2006 4) | 1,422+305 −390[18] |
L/Teff | |
| VY Canis Majoris | 1,420±120[19][20][21] | 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.[22] Potentially the largest known star.[20] There is a possibility that this size might be a bit overestimated (on the order of 1 sigma). Hence, the quoted radius might be just an upper limit.[19] |
| AH Scorpii | 1,411±124[23][24] | AD | Its angular diameter was re-measured at 5.05 ± 0.5 mas in 2023, which would yield a smaller radius of 1,227 R☉.[25] |
| CD–34°11794 | 1,409[26] | L/Teff | Oxygen-rich[27] red supergiant[28] and OH/IR star.[29] |
| RSGC1-F06 (FMR2006 6) | 1,382+298 −384[18] |
L/Teff | |
| S Persei | 1,364±6[30] | AD | Oxygen-rich[27][31] red supergiant.[32] Also called a hypergiant.[33] |
| VX Sagittarii | 1,360+250 −230[34] or 1,480+180 −160[24] |
AD | Either a very late-type red supergiant,[35][36] a particualarly large Super-AGB star,[34] or a possible but unlikely Thorne-Zyktow object.[34] Widely recognized as being among the largest known stars.[37] |
| NML Cygni | <1,350+195 −229[lower-alpha 3] |
AD | Surrounding dusty region is very complex making the radius hard to determine.[38] |
| Stephenson 2 DFK 2 | 1,300 ± 300[18] | L/Teff | Another red supergiant, Stephenson 2 DFK 1 has an estimated radius of 2,150 R☉. However, it is potentially not a member of the Stephenson 2 cluster and since its distance has been derived from its radial velocity, discrepancy with a trigonometric distance may be over 50%.[18][39] |
| Stephenson 2 DFK 49 | 1,300 ± 300[18] | L/Teff | A K-type star similar to the yellow hypergiant IRC +10420 that has left its red supergiant stage.[18] |
| HD 143183 (V558 Normae) | 1,261[26] | L/Teff | |
| PZ Cassiopeiae | 1,259 – 1,336[40] | L/Teff & AD | |
| Garnet Star (μ Cephei) | 1,259,[41] 1,420[42] or ~RBetelgeuse | L/Teff & AD | Widely recognised as being among the largest known stars.[37] Might be the largest star visible to the naked eye.[43] The higher radii estimate assume Mu Cephei is in the Cepheus OB2 OB association.[41][44] Other sources suggest Mu Cephei and Betelgeuse are likely similar in properties.[45][46] If so, Mu Cephei's radius would be comparable to that of Betelgeuse, which is between 650 and 800 R☉. |
| RSGC1-F10 (FMR2006 10) | 1,246+264 −337[18] |
L/Teff | |
| V354 Cephei | 1,245[26] | L/Teff | |
| Westerlund 1 W237 (Westerlund 1 BKS B) | 1,241±70,[47] 888[26] | L/Teff | Possibly a foreground giant.[48] |
| ST Cephei | 1,218[26] | L/Teff | |
| IRC -30312 | 1,204[26] | L/Teff | |
| IRC -10414 | ~1,200[49] | L/Teff | |
| RSGC1-F05 (FMR2006 5) | 1,185+254 −325[18] |
L/Teff | |
| V517 Monocerotis | 1,196+80 −159[50] – 1,208[26] |
L/Teff | |
| GCIRS 7 | 1,170±60,[51] 1,359,[52] 1,368[53] | AD & L/Teff | |
| Westerlund 1 W26 (Westerlund 1 BKS AS) | 1,165±58–1,221±120[47] | L/Teff | |
| [A72c] 16 | 1,157[26] | L/Teff | |
| WY Velorum A | 1,157[26] | L/Teff | A symbiotic binary.[54] |
| RSGC1-F08 (FMR2006 8) | 1,150+234 −297[18] |
L/Teff | |
| IRC -30303 | 1,147[26] | L/Teff | |
| RSGC1-F02 (FMR2006 2) | 1,128+238 −303[18] |
L/Teff | |
| Orbit of Jupiter | 1,114.5–1,115.8[10][lower-alpha 2] | Reported for reference | |
| V582 Cassiopeiae | 1,111[26] | L/Teff | |
| RW Cygni | 1,103+251 −177[55] |
AD | |
| RW Cephei | 1,100±40[56] | AD | A K-type hypergiant star that experienced a "great dimming" event in 2022, similar to Betelgeuse. |
| RT Carinae | 1,090[42] | L/Teff | |
| UU Persei | 1,079+9 −8[50] |
L/Teff | |
| LL Pegasi | 1,070[57] | L/Teff | |
| HD 126577 | 1,066+9 −32[50] |
L/Teff | |
| V766 Centauri Aa | 1,060–1,160[58] | ? | V766 Centauri Aa is a rare variable yellow hypergiant. |
| EV Carinae | 1,057[26] | L/Teff | Red supergiant.[59] An older study suggests an extremely high radius of 2,877 R☉.[60] |
| CM Velorum | 1,048[26] – 1,416.24+0.40 −0.96[50] |
L/Teff | |
| AG Camelopardalis | 1,048[26] | L/Teff | |
| SU Persei | 1,044+31 −21 – 1,139+34 −23,[30] |
AD | |
| SW Cephei | 1,035+75 −120[61] |
AD | |
| RSGC1-F11 (FMR2006 11) | 1,032+210 −267[18] |
L/Teff | |
| BC Cygni | 1,031[62] – 1,187+34 −37,[50] 1,062[26] |
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.[63] |
| MY Cephei | 1,028 ± 169 – 1,138 ± 387[64][lower-alpha 4] | L/Teff | |
| V530 Cassiopeiae | 1,017[26] | L/Teff | |
| V602 Carinae | 1,015[65] | AD | |
| VV Cephei A | 1,015[66] | AD | A red supergiant star orbited by a smaller B-type main-sequence star with a radius estimated between 13[67] and 25 R☉.[68] Widely recognised as being among the largest known stars.[37] Another estimate give a radius of 660 R☉[26] based on the Gaia DR3 distance of 1 kpc.[50] |
| U Lacertae A | 1,013[26] | L/Teff | |
| RSGC1-F13 (FMR2006 13) | 1,017+221 −286[18] |
L/Teff | |
| KW Sagittarii | 1,009±142[23][24] | AD | |
| Ve 4-64 | 1,007[26] | L/Teff | |
| RSGC1-F07 (FMR2006 7) | 1,007+215 −276[18] |
L/Teff | |
| V349 Carinae | 1,002+12 −74[50] |
L/Teff | |
| V674 Cephei | 999[26] | L/Teff | |
| RSGC1-F09 (FMR2006 9) | 996+210 −269[18] |
L/Teff | |
| IRAS 18111-2257 | ~990 – 1,200[69] | L/Teff | Estimated based on the bolometric luminosity (14,000–20,000 L☉) and assumed effective temperature of 2,000 K. Another period-luminosity-derived luminosity for this star results in a radius of 1,730 R☉.[69] |
| CIT 11 | 982[26] | L/Teff | |
| V381 Cephei Aa | 977[26] | L/Teff | |
| MSX6C G086.5890–00.7718 | (975+175 −183 – 1,035+186 −158)[70] – 1,196.91+6.31 −6.35[50] |
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. |
| V396 Centauri | 965[26] | L/Teff | |
| UW Aquilae | 964[26] | L/Teff | |
| RSGC1-F12 (FMR2006 12) | 955+204 −262[18] |
L/Teff | |
| RSGC1-F03 (FMR2006 3) | 942+179 −222[18] |
L/Teff | |
| V398 Cassiopeiae (HD 240275) | 941[26] | L/Teff | |
| IRC +60342 | 940[26] | L/Teff | |
| ψ1 Aurigae | 934[26] – 1,004[71] | L/Teff | |
| V645 Cephei | 920[26] | L/Teff | |
| UY Scuti | 909[26] | L/Teff | Once thought to be 1,708 ± 192 R☉[23] or 1,943 R☉.[60] |
| NR Vulpeculae | 908[26] – 923+62 −50[61] |
L/Teff | |
| KU Andromedae (IRC +40004) | 900[72] – 1,040[73] | L/Teff | |
| V774 Sagittarii | 889[26] | L/Teff | |
| V923 Centauri | 881[26] | L/Teff | |
| IRAS 20341+4047 | 880[26] | L/Teff | |
| IRAS 17418−2713 | 880[74] | L/Teff | |
| V540 Sagittarii | 880[26] | L/Teff | |
| V386 Cephei | 879[26] | L/Teff | |
| Trumpler 27-1 (CD–33°12241) | 876+5 −12[50] |
? | |
| TYC 3996-552-2 | 870[26] | L/Teff | |
| V1300 Aquilae (IRC −10529) | 860[72] – 1,100[73] | L/Teff | |
| Westerlund 1 W20 (Westerlund 1 BKS D) | 858±48[47] | L/Teff | |
| AZ Cygni | 856+20 −14 – 927+21 −15[30] |
AD | Estimated based on data from the CHARA array. Other radii of 890+21 −15 R☉ (2014), 895+21 −15 R☉ (2015) and 890+21 −15 R☉ (2016) are calculated based on the same data.[30] |
| V348 Velorum | 855[26] | L/Teff | |
| BI Cygni | 852+12 −9 – 908+12 −10[30] |
AD | |
| TW Carinae | 835[26] | L/Teff | |
| V358 Cassiopeiae | 835[26] | L/Teff | |
| DO 26226 | 826[26] | L/Teff | |
| HD 155737 | 823[26] | L/Teff | |
| 6 Geminorum | 821[30] | L/Teff | |
| RW Leonis Minoris | 820[75] – 1,000[73] | L/Teff | |
| HD 300933 | 806[26] | L/Teff | |
| [W61c] R 53 | 801[26] | L/Teff | |
| RT Ophiuchi | 801±217[76] | AD | |
| HD 95687 | 797[26] | L/Teff | |
| BO Carinae | 790±158[42] | L/Teff | |
| HD 62745 | 790[26] | L/Teff | |
| WX Piscium | 790[77] – 1,000[73] | L/Teff | |
| VR5–7 | 775 ± 65[78] | L/Teff | |
| V Cygni | 770[79] | L/Teff | |
| BD+63 3 | 770[26] | L/Teff | |
| CL Carinae | 770[26] | L/Teff | |
| RS Persei | 770±30,[80] 775+110 −85[61] |
AD | |
| V355 Cephei | 770±154[42] – 790[26] | L/Teff | |
| BD+63 270 | 769[26] | L/Teff | |
| V644 Cephei | 765[26] | L/Teff | |
| BM VIII 11 | 754[26] | L/Teff | |
| [SLN74] 2130 | 752[26] | L/Teff | |
| IRAS 10176-5802 | 751.2+0.4 −0.6[50] – (793+281 −152–849+172 −133)[70] |
L/Teff | Lower value based on the GSP Phot-Aeneas library using BR/RP spectra in Gaia DR3. Higher values based on the Gaia DR3 effective temperature and the luminosity of Levesque et al. (2005) and that of Messineo & Brown (2019). |
| HD 303250 | 750±150[42] | L/Teff | |
| V384 Persei | 750[72] – 940[73] | L/Teff | |
| GY Aquilae | 748[24] – 920[81] | AD | |
| UU Pegasi | 742±193[76] | AD | |
| IM Cassiopeiae | 740[26] | L/Teff | |
| Stephenson 2 DFK 10 | 730[18] | L/Teff | |
| VdBH 222#566 | 725[82] | L/Teff | May be larger at 912 R☉, however this is unlikely due to the luminosity does not match with the H-R diagram where the temperature was calculated. |
| HD 105563 A | 723[26] | L/Teff | |
| Westerlund 1 W75 (Westerlund 1 BKS E) | 722±36[47] | L/Teff | |
| V1111 Ophiuchi (IRC +10365) | 720[72] – 900[73] | L/Teff | |
| XX Persei | 718+80 −56[61] |
AD | |
| RX Telescopii | 716[26] | L/Teff | |
| V Camelopardalis | 716±185[76] | AD | |
| CD–61°3575 | 716[26] | L/Teff | |
| AS Cephei | 713[26] | L/Teff | |
| V770 Cassiopeiae (BD+60 299) | 713[26] | L/Teff | |
| AZ Cephei | 712[26] | L/Teff | |
| R Leporis (Hind's Crimson Star) | 710 – 910[83] | AD | |
| MZ Puppis | 708[26] | L/Teff | |
| GP Cassiopeiae | 707[26] – 771.74+0.23 −0.86[50] |
L/Teff | |
| GCIRS 12N | 703 ± 107[78] | L/Teff | |
| V528 Carinae | 700±140[42] | L/Teff | |
| The following well-known stars are listed for the purpose of comparison. | |||
| Antares (α Scorpii A) | 680[84] | AD | Fourteenth brightest star in the night sky.[85] Widely recognised as being among the largest known stars.[37] |
| Betelgeuse (α Orionis) | 640,[86] 764+116 −62,[87] 782 ± 55[88] |
AD & SEIS | Tenth brightest star in the night sky.[85] Widely recognised as being among the largest known stars,[37] radius decreased to ~500 R☉ during the 2020 great dimming event.[89] |
| R Horologii | 630[72] | L/Teff | A red giant star with one of the largest ranges in brightness known of stars in the night sky visible to the unaided eye. Despite its large radius, it is less massive than the Sun. |
| V382 Carinae | 616±69[90] | AD | A yellow hypergiant, one of the rarest types of stars. |
| 119 Tauri (CE Tauri, Ruby Star) | 587 – 593[91] | AD | |
| ρ Cassiopeiae | 564±67 or 700±112[92] | AD | A yellow hypergiant star, similar to V382 Carinae, that is also visible to the naked eye. |
| CW Leonis | 560[93] | L/Teff | The nearest carbon star. |
| V838 Monocerotis | 464[94] | L/Teff | During the 2002 Red Nova, the star's radius may have increased up to 3,190 R☉.[95] |
| V509 Cassiopeiae | 449±20[90] | AD | A variable yellow hypergiant whose size varied from around 680 R☉ in 1950–1970 to 910 R☉ in 1977, and later decreased to 390 R☉ in the 1990s.[96] |
| Pistol Star (V4647 Sagittarii) | 420[97] | L/Teff | One of the most luminous stars known. |
| Mira (ο Ceti A) | 332–402[98] | AD | Prototype of the Mira variables. |
| Orbit of Mars | 322–323.1[10][lower-alpha 2] | Reported for reference | |
| R Doradus | 298±21[99] | AD | The extrasolar star with the largest apparent size. |
| Rasalgethi (α Herculis A) | 284±60 (264–303)[100] | L/Teff | |
| Cygnus OB2#12 | 246[101] | ? | One of the most massive and luminous stars known. |
| Orbit of Earth (~1 AU) | 214[10][lower-alpha 2] | Reported for reference | |
| Suhail (λ Velorum) | 211±6[102] | AD | |
| Wezen (δ Canis Majoris) | 188[103] | L/Teff | Thirty-sixth brightest star in the night sky.[85] |
| Enif (ε Pegasi) | 178[103] | L/Teff | |
| Orbit of Venus | 158.6[10][lower-alpha 2] | Reported for reference | |
| η Carinae A | 128 – 742[104] | OD | During the 1843 Great Eruption, the star's radius may have increased up to 4,319–6,032 R☉.[105] |
| Deneb (α Cygni) | 107[106][lower-alpha 5] – 203±17[107] | AD & ? | Eighteenth brightest star in the night sky.[85] |
| Orbit of Mercury | 82.9–84.6[10][lower-alpha 2] | Reported for reference | |
| Rigel (β Orionis A) | 74.1+6.1 −7.3[108] |
AD | Seventh brightest star in the night sky. |
| Canopus (α Carinae) | 73.3[109] | AD | Second brightest star in the night sky. |
| Gacrux (γ Crucis) | 73[110] | L/Teff | Twenty-sixth brightest star in the night sky. |
| Polaris (α Ursae Minoris) | 46.27±0.42[111] | AD | The current star in the North Pole. It is a Classical Cepheid variable, and the brightest example of its class. |
| Aldebaran (α Tauri A) | 45.1±0.1[112] | AD | Fourteenth brightest star in the night sky. |
| Arcturus (α Boötis) | 25.4 ± 0.2[113] | AD | This is the nearest red giant to the Earth, and the fourth brightest star in the night sky. |
| Pollux (β Geminorum) | 9.06 ± 0.03[108] | AD | The nearest giant star to the Earth. |
| Spica (α Virginis A) | 7.47±0.54[114] | One of the nearest supernova candidates and the sixteenth-brightest star in the night sky. | |
| Regulus (α Leonis A) | 4.16 × 3.14[115] | The nearest B-type star to the Earth. | |
| Vega (α Lyrae) | 2.726±0.006 × 2.418±0.012[116] | AD | Fifth brightest star in the night sky.[85] |
| Altair (α Aquilae) | 2.01 × 1.57[117] | Twelfth brightest star in the night sky. | |
| Sirius (α Canis Majoris A) | 1.713[118] | AD | The brightest star in the night sky. |
| Rigil Kentaurus (α Centauri A) | 1.2175[119] | AD | Third brightest star in the night sky. |
| Sun | 1 | The largest object in the Solar System. | |
Magellanic Clouds
| Star name | Solar radius (R☉) | Galaxy | Method[lower-alpha 1] | Notes |
|---|---|---|---|---|
| Theoretical limit of star size (Large Magellanic Cloud) | ≳1,550[11] | L/Teff | Estimated by measuring the fraction of red supergiants at higher luminosities in a large sample of stars. Assumes an effective temperature of 3,545 K. Reported for reference | |
| WOH G64 A | 1,540[12][13][14][15][16] ± 77[12] | Large Magellanic Cloud | L/Teff | Surrounded by a large dust cloud.[120] Possibly the largest known star.[12][13][17][14] |
| MSX LMC 839 | 1,526[121] | Large Magellanic Cloud | L/Teff | |
| HV 888 (WOH S140) | 1,509[122] | Large Magellanic Cloud | L/Teff | |
| IRAS 04516–6902 | 1,502[15] | Large Magellanic Cloud | L/Teff | |
| W60 A27 | 1,444[15] | Large Magellanic Cloud | L/Teff | |
| IRAS 05280–6910 | 1,367[123] | Large Magellanic Cloud | L/Teff | The most reddened object in the Large Magellanic Cloud.[15] |
| IRAS 04509–6922 | 1,339[15] | Large Magellanic Cloud | L/Teff | |
| IRAS 05346-6949 | 1,211[124] | Large Magellanic Cloud | L/Teff | It has an estimated mass-loss rate of 0.0017 M☉ (566 Earths) per year, the highest for any star.[124] |
| W60 B90 (WOH S264) | 1,210[125] | Large Magellanic Cloud | L/Teff | Has an unusually high metallicity and velocity.[125] |
| HV 2242 | 1,160[126] – 1,180[127] | Large Magellanic Cloud | L/Teff | |
| MSX SMC 018 | 1,119[124] | Small Magellanic Cloud | L/Teff | |
| WOH S338 | 1,100[126] | Large Magellanic Cloud | L/Teff | |
| MSX LMC 589 | 1,051[121] | Large Magellanic Cloud | L/Teff | |
| Theoretical limit of star size (Small Magellanic Cloud) | ≳1,050[11] | L/Teff | Estimated by measuring the fraction of red supergiants at higher luminosities in a large sample of stars. Assumes an effective temperature of 3,850 K. Reported for reference | |
| IRAS 05402-6956 | 1,032[123] | Large Magellanic Cloud | L/Teff | |
| Sk -69 148 | 1,006[128] | Large Magellanic Cloud | L/Teff | A yellow hypergiant. |
| HV 2450 | 1,000+2 −1[129]–1,071[129] |
Large Magellanic Cloud | L/Teff | A yellow hypergiant. |
| UCAC2 2674864 (HV 2834) | 990+115 −100[13] |
Large Magellanic Cloud | L/Teff | |
| HV 2362 | 982[127] – 1,030[126] | Large Magellanic Cloud | L/Teff | |
| MG73 59 | 979[130] | Large Magellanic Cloud | L/Teff | A yellow supergiant. |
| HD 268757 | 979[130] | Large Magellanic Cloud | L/Teff | A G8 yellow hypergiant. |
| LMC 147199 | 939[127] – 990[126] | Large Magellanic Cloud | L/Teff | |
| LMC 23095 | 926[121] – 1,280[127] | Large Magellanic Cloud | L/Teff | |
| SP77 31–16 | 923±28[129] | Large Magellanic Cloud | L/Teff | A yellow hypergiant. |
| LMC 66778 | 915[127] – 990[126] | Large Magellanic Cloud | L/Teff | |
| WOH S457 | 902±45[131] | Large Magellanic Cloud | L/Teff | |
| IRAS 04498-6842 (LI-LMC 60) | 898[123] – 1,137[121] – 1,765,[15] 1,224[127] | Large Magellanic Cloud | L/Teff | Lower value derived from fitting models that assume the star's effective temperature to be 3,400 K. Higher value based on the measured effective temperature from van Loon et al. (2005). A newer paper estimates parameters that would result in a radius of 1,765 R☉.[15] |
| HV 12185 | 890+55 −65[13] |
Large Magellanic Cloud | L/Teff | |
| HV 12793 | 880+45 −65[13] |
Large Magellanic Cloud | L/Teff | |
| WOH S57 | 875+70 −60[13] |
Large Magellanic Cloud | L/Teff | |
| SP77 28–2 | 825±60[13] | Large Magellanic Cloud | L/Teff | |
| SP77 22–9 | 823[127] – 850[126] | Large Magellanic Cloud | L/Teff | |
| Z Doradus | 824±108[131]–956[121] | Large Magellanic Cloud | L/Teff | |
| SP77 40–7 | 778[127] – 810[126] | Large Magellanic Cloud | L/Teff | |
| W61 19–24 | 780+50 −70[13] |
Large Magellanic Cloud | L/Teff | |
| WOH S28 | 780[126] | Large Magellanic Cloud | L/Teff | |
| SP77 48–6 | 768[132] | Large Magellanic Cloud | L/Teff | |
| WOH S452 | 762±275[131] | Large Magellanic Cloud | L/Teff | |
| WOH S438 | 757±211[131] | Large Magellanic Cloud | L/Teff | |
| LMC 139027 | 751[127] – 790[126] | Large Magellanic Cloud | L/Teff | |
| SP77 45–16 | 749[127] – 800[126] | Large Magellanic Cloud | L/Teff | |
| SP77 54–27 | 750[126] – 758[127] – 800[126] | Large Magellanic Cloud | L/Teff | |
| SP77 39–17 | 736[127] – 760[126] | Large Magellanic Cloud | L/Teff | |
| HD 269723 | 734±17,[129] 814[130]–829[132] | Large Magellanic Cloud | L/Teff | A yellow hypergiant. |
| PMMR 64 | 730+75 −65[13] |
Small Magellanic Cloud | L/Teff | |
| LH 43–15 | 719[127] – 740[126] | Large Magellanic Cloud | L/Teff | |
| PMMR 116 | 717[132] | Small Magellanic Cloud | L/Teff | |
| MSX SMC 055 | 702[133]–1,557+215 −130[121] |
Small Magellanic Cloud | L/Teff | A super-AGB candidate. |
| SP77 48–6 | 700+29 −28[129] |
Large Magellanic Cloud | L/Teff | A yellow hypergiant. |
| The following well-known stars are listed for the purpose of comparison. | ||||
| HV 2112 | 675 – 1,193[134] | Small Magellanic Cloud | L/Teff | It has been previously considered to be a possible Thorne–Żytkow object.[134] |
| HV 11417 | 673[121]–798[127] | Small Magellanic Cloud | L/Teff | Candidate Thorne-Zytkow object.[134] |
| HD 269953 | 647[130]–720[132] | Large Magellanic Cloud | L/Teff | A yellow hypergiant. |
| HD 33579 | 471[132] | Large Magellanic Cloud | L/Teff | The brightest star in the Large Magellanic Cloud. |
| S Doradus | 100[135] | Large Magellanic Cloud | L/Teff | A luminous blue variable in the S Doradus instability strip. |
| HD 37974 | 99[136] | Large Magellanic Cloud | L/Teff | An unusual blue hypergiant with a large dusty disk.[136] |
| R136a1 | 42.7+1.6 −0.9[137] |
Large Magellanic Cloud | L/Teff | One of the most luminous and most massive stars. |
| BAT 99-98 | 37.5[138] | Large Magellanic Cloud | L/Teff | One of the most luminous and most massive stars. |
| HD 5980 A | 24[139] | Small Magellanic Cloud | L/Teff | A luminous blue variable and one of the most luminous stars. |
Andromeda (M31) and Triangulum (M33) galaxies
| Star name | Solar radius (R☉) | Galaxy | Method[lower-alpha 1] | Notes |
|---|---|---|---|---|
| Theoretical limit of star size (Andromeda Galaxy) | ≳1,750[11] | L/Teff | Estimated by measuring the fraction of red supergiants at higher luminosities in a large sample of stars. Assumes an effective temperature of 3,625 K. Reported for reference | |
| Theoretical limit of star size (Triangulum Galaxy) | ≳1,500[11] | L/Teff | Estimated by measuring the fraction of red supergiants at higher luminosities in a large sample of stars. Assumes an effective temperature of 3,605 K. Reported for reference | |
| LGGS J004428.48+415130.9 | 1,410[140] | Andromeda Galaxy | L/Teff | |
| LGGS J013418.56+303808.6 | 1,363[141] | Triangulum Galaxy | L/Teff | |
| M31-1775 | 1,254[142] | Andromeda Galaxy | L/Teff | |
| M31-1515 | 1,112[142] | Andromeda Galaxy | L/Teff | Within a binary star system with an OB companion.[142] |
| M33-2747 | 1,057[142] | Triangulum Galaxy | L/Teff | |
| M31-1372 | 926[142] | Andromeda Galaxy | L/Teff | |
| M31-504 | 919[142] | Andromeda Galaxy | L/Teff | |
| M31-1414 | 893[142] | Andromeda Galaxy | L/Teff | |
| M33-113 | 890[142] | Triangulum Galaxy | L/Teff | |
| M33-453 | 836[142] | Triangulum Galaxy | L/Teff | |
| M33-374 | 824[142] | Triangulum Galaxy | L/Teff | |
| M33-920 | 799[142] | Triangulum Galaxy | L/Teff | |
| M33-255 | 797[142] | Triangulum Galaxy | L/Teff | |
| M31-2338 | 792[142] | Andromeda Galaxy | L/Teff | |
| M31-2420 | 786[142] | Andromeda Galaxy | L/Teff | |
| LGGS J004255.95+404857.5 | 785[143] | Andromeda Galaxy | L/Teff | |
| M31-2252 | 783[142] | Andromeda Galaxy | L/Teff | |
| M31-1494 | 758[142] | Andromeda Galaxy | L/Teff | |
| M31-1410 | 772[142] | Andromeda Galaxy | L/Teff | |
| M31-689 | 767[142] | Andromeda Galaxy | L/Teff | |
| LGGS J004124.80+411634.7 | 760, 1,205, 1,240[143] | Andromeda Galaxy | L/Teff | |
| M31-1621 | 743[142] | Andromeda Galaxy | L/Teff | |
| LGGS J013349.86+303246.1 | 710[144]–795[141] | Triangulum Galaxy | L/Teff | A yellow supergiant. |
| The following well-known stars are listed for the purpose of comparison. | ||||
| Var 83 | 150[145] | Triangulum Galaxy | L/Teff | A luminous blue variable and one of the most luminous stars in M33. |
Other galaxies (within the Local Group)
| Star name | Solar radius (R☉) | Galaxy | Method[lower-alpha 1] | Notes |
|---|---|---|---|---|
| NGC 6822-52 | 1,053[146] | NGC 6822 | L/Teff | |
| Sextans A 10 | 995±130[147] | Sextans A | L/Teff | |
| NGC 6822-RSG 19 | 928[148] | NGC 6822 | L/Teff | |
| WLM 02 | 883+284 −167[149] |
WLM | L/Teff | |
| Sextans A 5 | 870±145[147] | Sextans A | L/Teff | |
| NGC 6822-RSG 26 | 866[148] | NGC 6822 | L/Teff | |
| NGC 6822-70 | 860[146] | NGC 6822 | L/Teff | |
| NGC 6822-RSG 12 | 837[148] | NGC 6822 | L/Teff | |
| NGC 6822-55 | 830[146] | NGC 6822 | L/Teff | |
| NGC 6822-103 | 787[146] | NGC 6822 | L/Teff | |
| IC 10-26089 | 769[146] | IC 10 | L/Teff | |
| NGC 6822-RSG 9 | 763[148] | NGC 6822 | L/Teff | |
| NGC 6822-RSG 6 | 712[148] | NGC 6822 | L/Teff | |
| Sextans A 7 | 710±100[147] | Sextans A | L/Teff | |
| The following well-known stars are listed for the purpose of comparison. | ||||
| AT 2018akx | 211[150] | NGC 3109 | L/Teff | It is a LBV,[151] and is the second brightest star in NGC 3109. |
| NGC 6822-WR 12 | 3.79[152] | NGC 6822 | L/Teff | A Wolf-Rayet star, one of the hottest known stars. |
Outside the Local Group (inside the Virgo supercluster)
| Star name | Solar radius (R☉) | Galaxy | Group | Method[lower-alpha 1] | Notes |
|---|---|---|---|---|---|
| NGC 300-125 | 1,504+176 −157[153] |
NGC 300 | NGC 55 Group | L/Teff | Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.[153] |
| NGC 247-154 | 1,503+79 −75[153] |
NGC 247 | Sculptor Group | L/Teff | Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.[153] |
| NGC 7793-34 | 1,392+157 −160[153] |
NGC 7793 | Sculptor Group | L/Teff | Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.[153] |
| NGC 55-40 | 1,286 +116−106[153] | NGC 55 | NGC 55 Group | L/Teff | Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.[153] |
| NGC 300-154 | 1,200 +123−111[153] | NGC 300 | NGC 55 Group | L/Teff | Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.[153] |
| NGC 300-114 | 1,181 +123−111[153] | NGC 300 | NGC 55 Group | L/Teff | Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.[153] |
| NGC 300-199 | 1,181 +120−109[153] | NGC 300 | NGC 55 Group | L/Teff | Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.[153] |
| NGC 300-153 | 1,173 +120−109[153] | NGC 300 | NGC 55 Group | L/Teff | Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.[153] |
| NGC 300-150 | 1,167 +119−107[153] | NGC 300 | NGC 55 Group | L/Teff | Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.[153] |
| NGC 253-2006 | 1,167 +75−70[153] | Sculptor Galaxy | Sculptor Group | L/Teff | Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.[153] |
| SPIRITS 14atl | 1,134–1,477[154] | Messier 83 | Centaurus A/M83 Group | L/Teff | |
| NGC 300-59 | 1,133 +146−129[153] | NGC 300 | NGC 55 Group | L/Teff | Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.[153] |
| NGC 7793-86 | 1,127 +94−109[153] | NGC 7793 | Sculptor Group | L/Teff | Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.[153] |
| NGC 300-263 | 1,108 +113−102[153] | NGC 300 | NGC 55 Group | L/Teff | Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.[153] |
| NGC 247-447 | 1,101 +58−56[153] | NGC 247 | Sculptor Group | L/Teff | Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.[153] |
| SPIRITS 15ahp | 1,098[154] | NGC 2403 | M81 Group | L/Teff | |
| NGC 300-240 | 1,088 +112−101[153] | NGC 300 | NGC 55 Group | L/Teff | Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.[153] |
| NGC 7793-86 | 1,078 +69−64[153] | NGC 7793 | Sculptor Group | L/Teff | Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.[153] |
| NGC 300-173 | 1,063 +84−77[153] | NGC 300 | NGC 55 Group | L/Teff | Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.[153] |
| NGC 300-340 | 1,036 +105−95[153] | NGC 300 | NGC 55 Group | L/Teff | Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.[153] |
| NGC 300-346 | 1,023 +139−128[153] | NGC 300 | NGC 55 Group | L/Teff | Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.[153] |
| NGC 247-533 | 1,004 +66−62[153] | NGC 247 | Sculptor Group | L/Teff | Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.[153] |
| NGC 300-351 | 992 +115−102[153] | NGC 300 | NGC 55 Group | L/Teff | Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.[153] |
| NGC 300-524 | 987 +77−72[153] | NGC 300 | NGC 55 Group | L/Teff | Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.[153] |
| NGC 55-135 | 964 +99−89[153] | NGC 55 | NGC 55 Group | L/Teff | Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.[153] |
| NGC 55-93 | 955 +49−47[153] | NGC 55 | NGC 55 Group | L/Teff | Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.[153] |
| NGC 7793-539 | 948[153] | NGC 7793 | Sculptor Group | L/Teff | Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.[153] |
| NGC 55-87 | 948 +109−98[153] | NGC 55 | NGC 55 Group | L/Teff | Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.[153] |
| NGC 55-146 | 921 +49−46[153] | NGC 55 | NGC 55 Group | L/Teff | Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.[153] |
| NGC 300-273 | 921 +94−85[153] | NGC 300 | NGC 55 Group | L/Teff | Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.[153] |
| NGC 300-186 | 915 +72−65[153] | NGC 300 | NGC 55 Group | L/Teff | Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.[153] |
| NGC 55-200 | 905 +59−55[153] | NGC 55 | NGC 55 Group | L/Teff | Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.[153] |
| NGC 55-152 | 895 +58−54[153] | NGC 55 | NGC 55 Group | L/Teff | Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.[153] |
| NGC 300-413 | 861 +66−61[153] | NGC 300 | NGC 55 Group | L/Teff | Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.[153] |
| NGC 55-174 | 856 +65−61[153] | NGC 55 | NGC 55 Group | L/Teff | Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.[153] |
| NGC 55-75 | 836 +81−111[153] | NGC 55 | NGC 55 Group | L/Teff | Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.[153] |
| NGC 300-545 | 824 +104−93[153] | NGC 300 | NGC 55 Group | L/Teff | Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.[153] |
| NGC 247-2912 | 821 +54−51[153] | NGC 247 | Sculptor Group | L/Teff | Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.[153] |
| NGC 55-216 | 801 +102−89[153] | NGC 55 | NGC 55 Group | L/Teff | Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.[153] |
| NGC 247-1471 | 798 +52−48[153] | NGC 247 | Sculptor Group | L/Teff | Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.[153] |
| NGC 300-499 | 796 +89−108[153] | NGC 300 | NGC 55 Group | L/Teff | Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.[153] |
| NGC 300-379 | 744 +56−52[153] | NGC 300 | NGC 55 Group | L/Teff | Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.[153] |
| NGC 300-838 | 744 +57−53[153] | NGC 300 | NGC 55 Group | L/Teff | Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.[153] |
| NGC 55-149 | 738 +47−55[153] | NGC 55 | NGC 55 Group | L/Teff | Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.[153] |
| NGC 55-194 | 730 +46−44[153] | NGC 55 | NGC 55 Group | L/Teff | Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.[153] |
| NGC 55-270 | 728 +38−36[153] | NGC 55 | NGC 55 Group | L/Teff | Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.[153] |
| NGC 300-1047 | 724 +65−59[153] | NGC 300 | NGC 55 Group | L/Teff | Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.[153] |
| NGC 247-3231 | 719 +56−51[153] | NGC 247 | Sculptor Group | L/Teff | Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.[153] |
| NGC 247-2966 | 719 +56−52[153] | NGC 247 | Sculptor Group | L/Teff | Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.[153] |
| NGC 55-245 | 717 +55−50[153] | NGC 55 | NGC 55 Group | L/Teff | Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.[153] |
| NGC 300-1068 | 716 +64−58[153] | NGC 300 | NGC 55 Group | L/Teff | Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.[153] |
| NGC 300-1081 | 712 +54−51[153] | NGC 300 | NGC 55 Group | L/Teff | Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius.[153] |
| The following well-known stars are listed for the purpose of comparison. | |||||
| Holmberg IX V1 A | 337[155] | Holmberg IX | M81 Group | L/Teff | Primary star of a yellow supergiant contact binary. |
| Holmberg IX V1 B | 306[155] | Holmberg IX | M81 Group | L/Teff | Secondary star of a yellow supergiant contact binary. |
| NGC 2363-V1 | 194–356[156] | NGC 2366 | M81 Group | L/Teff | |
Outside the Virgo supercluster
Note that this list does not include the candidate JWST dark stars, with estimated radii of up to 61 Astronomy:astronomical unit|astronomical units (13,000 R☉)[157] or quasi-stars, with theoretical models suggesting that they could reach radii of up to 40,700 solar radii (189 au).[158]
| Star name | Solar radius (R☉) | Galaxy | Group | Method[lower-alpha 1] | Notes |
|---|---|---|---|---|---|
| W2 A | 1,182[159] | Warhol Arc | MACS J0416.1-2403 | L/Teff | W2 A is the primary star in a binary system consisting of a red supergiant and a B-type supergiant, located at redshift z = 0.94. |
| Quyllur | 965[160] | ACT-CL J0102-4915 | L/Teff | Likely the first red supergiant star at cosmological distances and is also discovered by James Webb Space Telescope. | |
| The following well-known stars are listed for the purpose of comparison. | |||||
| Godzilla | 430–2,365[161] | Sunburst galaxy | PSZ1 G311.65-18.48 | L/Teff | The most luminous known star.[162] |
| Mothra | 271[163] | LS1 | MACS J0416.1-2403 | L/Teff | A binary star at cosmological distances. |
Transient events
During some transient events, such as red novae or LBV eruptions the star's radius can increase by a significant amount.
| Star or transient event name | Solar radius (R☉) | Year | Galaxy | Group | Method | Notes |
|---|---|---|---|---|---|---|
| AT 2017jfs | >33,000[164] | 2017 | NGC 4470 | L/Teff | ||
| SNhunt151 | 16,700[165] | 2014 | UGC 3165 | LDC 331 | L/Teff | |
| SN 2015bh | 16,400±2,600[166] | 2015 | NGC 2770 | LDC 616 | L/Teff | |
| AT 2018hso | 10,350[167] | 2018 | NGC 3729 | M109 Group | L/Teff | |
| AT 2023clx | 6,800[168] | 2023 | NGC 3799 | nest 101314 | L/Teff | |
| M51 OT2019-1 | 5,500[169] | 2019 | Whirlpool Galaxy | M51 Group | L/Teff | |
| η Carinae | 4,319 – 6,032[105] | 1845 | Milky Way | Local Group | L/Teff | During the outburst, the star became the second brightest star in sky, reaching an apparent magnitude of between −0.8 and −1.0.[170] |
| AT 2010dn | 4,130[171] | 2010 | NGC 3180 | LDC 743 | L/Teff | |
| SN 2011fh | 3,980[172] | 2011 | NGC 4806 | Abell 3528 | L/Teff | |
| AT 2014ej | 3,600[173] | 2014 | NGC 7552 | Grus Quartet | L/Teff | |
| V838 Monocerotis | 3,190[95] | 2002 | Milky Way | Local Group | L/Teff | |
| SN2008S | 3,020[171] | 2008 | NGC 6946 | NGC 6946 Group | L/Teff | |
| SNhunt120 | 2,900[174][173] | 2012 | NGC 5775 | Virgo Cluster | L/Teff | |
| AT 2017be | 2,000[175] | 2017 | NGC 2537 | L/Teff | ||
| PHL 293B star | 1,348 – 1,463[176] | 2002 | PHL 293B | L/Teff | ||
| SNhunt248 | ~850[177] | 2014 | NGC 5806 | NGC 5846 Group | L/Teff | |
| SN 2002kg | 704[178] | 2002 | NGC 2403 | M81 Group | L/Teff | |
| R71 | 500[179] | 2012 | Large Magellanic Cloud | Local Group | L/Teff | |
| SN 2000ch | 500[180] | 2000 | NGC 3432 | LDC 743 | L/Teff | |
| Godzilla | 430 – 2,365[161] | 2015 | Sunburst galaxy | L/Teff | ||
| AT 2016blu | ~330[181] | 2012 – 2022 | NGC 4559 | Coma I Group | L/Teff | 19 outbursts were detected between 2012 and 2022. The star was likely relatively stable the decade before since no outbursts were detected from 1999 – 2009.[181] |
SN Progenitors
| Star or supernova name | Solar radius (R☉) | Year | Galaxy | Group | Method | Notes |
|---|---|---|---|---|---|---|
| SN 2025pht | 1,850 ± 340 – 2,620 ± 480[182] | 2025 | NGC 1637 | L/Teff | ||
| SN 2020xva | 1,520[183] | 2020 | SDSS J173209.23+533908.4 | L/Teff | ||
| SN 2019ust | 1,440[183] | 2019 | UGC 548 | [TKT2016] 54 | L/Teff | |
| N6946-BH1 | 1,216-2,720[184] | 2008 | NGC 6946 | LDC 1412 | L/Teff | Not a true supernova and was a failed supernova. |
| SN 2021ibn | 1,200[183] | 2021 | 2MASX J08501445+3701127 | L/Teff | ||
| SN 2020afdi | 1,200[183] | 2020 | NGC 5836 | L/Teff | ||
| SN 2002hh | 1,184-1,904[185] | 2002 | NGC 6946 | LDC 1412 | L/Teff | |
| SN 2018fif | 1,174[186] | 2018 | UGC 85 | LGG 485 | L/Teff | |
| SN 1999an | 1,131-1,492[185] | 1999 | IC 755 | Virgo Cluster | L/Teff | |
| SN 2019eoh | 1,100±130[183] | 2019 | IC 4145 | L/Teff | ||
| SN 2017eaw | 1,000-2,000[187] | 2017 | NGC 6946 | LDC 1412 | L/Teff | |
| SN 2020faa | 1,000[188] | 2020 | 2MASS J14470904+7244157 | L/Teff | ||
| SN 2023ixf | 912+227 −222[189]–1,060±30[190] |
2023 | Pinwheel galaxy | M101 Group | L/Teff | |
| SN 2004et | 893-976[185] | 2004 | NGC 6946 | LDC 1412 | L/Teff | |
| SN 2019oxn | 780±120[183] | 2019 | SDSS J175113.25+512300.1 | L/Teff | ||
| SN 2018aoq | 742[185] | 2018 | NGC 4151 | LDC 867 | L/Teff | |
| NGC3021-CANDIDATE-1 | 722[191] | 2005 | NGC 3021 | LDC 676 | L/Teff | Not a true supernova and was a failed supernova. |
| SN 1999br | 717-945[185] | 1999 | NGC 4900 | Virgo Cluster | L/Teff | |
| SN 2020jfo | 700±10[192] | 2020 | Messier 61 | Virgo Cluster | L/Teff | |
| SN 2009hd | 686[185] | 2009 | Messier 66 | M66 Group | L/Teff | Progenitor was similar to V915 Scorpii. |
| SN 1999em | 663-942[185] | 1999 | NGC 1637 | [TSK2008] 975 | L/Teff | |
| SN 2009md | 663[185] | 2009 | NGC 3389 | LGG 214 | L/Teff | |
| SN 2012ec | 625[185] | 2012 | NGC 1084 | NGC 1052 Group | L/Teff | |
| SN 1999gi | 593-783[185] | 1999 | NGC 3184 | LDC 743 | L/Teff | |
| SN 2006my | 585-941[185] | 2006 | NGC 4651 | Virgo Cluster | L/Teff | |
| SN 2007aa | 559-737[185] | 2007 | NGC 4030 | Virgo Cluster | L/Teff | |
| SN 2012aw | 549-882[185] | 2012 | Messier 95 | LGG 217 | L/Teff | |
| SN 2004A | 539-866[185] | 2004 | NGC 6207 | [TKS2008] 816 | L/Teff | |
| SN 2001du | 534-744[185] | 2001 | NGC 1365 | Fornax Cluster | L/Teff | |
| SN 2012A | 513-588[185] | 2012 | NGC 3239 | LDC 778 | L/Teff | |
| SN 2013ej | 512[185] | 2013 | Messier 74 | M74 Group | L/Teff | |
| SN 2009kr | 504-2,182[185] | 2009 | NGC 1832 | NGC 1832 Group | L/Teff | Progenitor was a RSG or YSG. |
| SN 2020cxd | 500[183] | 2020 | NGC 6395 | LDC 1246 | L/Teff | |
| SN 2024abfl | 499-592[193] | 2024 | NGC 2146 | L/Teff | ||
| SN 2008bk | 494-567[185] | 2008 | NGC 7793 | Sculptor Group | L/Teff | |
| SN 2020fqv | 490[183] | 2020 | NGC 4568 | Virgo Cluster | L/Teff | |
| SN 2024ggi | 477[185] | 2024 | NGC 3621 | [TSK2008] 310 | L/Teff | |
| SN 2008cn | 439[185] | 2008 | NGC 4603 | LGG 301 | L/Teff | Progenitor was a YSG. |
| SN 2023axu | 417±28[194] | 2023 | NGC 2283 | [TSK2008] 995 | L/Teff | |
| SN 2005cs | 409[185] | 2005 | Whirlpool Galaxy | M51 Group | L/Teff | |
| SN 2004dg | 407-654[185] | 2004 | NGC 5806 | NGC 5846 Group | L/Teff | |
| SN 2003gd | 384[195] | 2003 | Messier 74 | M74 Group | L/Teff | |
| SN 2006bc | 378-608[185] | 2006 | NGC 2397 | LGG 147 | L/Teff | |
| SN 2006ov | 326-524[185] | 2006 | Messier 61 | Virgo Cluster | L/Teff | |
| SN 2022acko | 323-520[185] | 2022 | NGC 1300 | LGG 90 | L/Teff | |
| SN 2003gm | 216-278[196] | 2003 | NGC 5334 | L/Teff | ||
| SN 2005gl | 201[197] | 2005 | NGC 266 | LGG 14 | L/Teff | Progenitor was a LBV. |
| SN 2013cu | >144, 368[198] | 2013 | UGC 9379 | L/Teff | Progenitor was either a YHG or LBV. | |
| SN 2020bio | 100-1,500[199] | 2020 | NGC 5390 | LGG 361 | L/Teff | |
| SN 1961V | 100[200] | 1961 | NGC 1058 | NGC 1023 Group | L/Teff | May be the hyper-eruption of a LBV. |
| SN 2021agco | 78.37+25.59 −19.94[201] |
2021 | UGC 3855 | LDC 506 | L/Teff | Nearest ultrastripped supernova known. |
| SN 1987A | 41.15[202] | 1987 | Large Magellanic Cloud | Local Group | L/Teff | |
| iPTF13bvn | 9.8[203] | 2013 | NGC 5806 | NGC 5846 Group | L/Teff | Progenitor was WR star. |
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.
| Name | Angular diameter (mas) |
Angular diameter type[lower-alpha 6] | Distance (light-years) |
Spectral type[204] | Notes |
|---|---|---|---|---|---|
| Sun | 2,000,000 | 0.000016 | G2V | The largest star by angular diameter. | |
| R Doradus | 51.18±1.24[99] | LD |
179±10[99] |
M8III:e | The largest star by angular diameter apart from the Sun. |
| Betelgeuse (α Orionis) |
42.28±0.43[87] | LD |
408–540+98−49[87] |
M1-M2Ia-Iab | |
| Antares (α Scorpii A) |
37.31±0.09[205] | LD | 553.5±93.9[206] | M1.5Iab | |
| Mira (ο Ceti) |
28.9±0.3 – 34.9±0.4[207] | Ross | 299±33[206] | M5-M9IIIe | The angular diameter vary during Mira's pulsations. |
| Tiaki (β Gruis) |
28.8±0.6[208] | ? | 177±4[206] | M4.5III | |
| Gacrux (γ Crucis) |
24.7[110] | ? | 88.6±0.4[206] | M3.5III | |
| Rasalgethi (α Herculis) |
23.95±5.03[100] | Est | 359±52[206] | M5Ib-II | |
| R Hydrae | 23.7±1[24] | ? | 482±33[24] | M6-9e | |
| Arcturus (α Boötis) |
21.06±0.17[209] | LD | 36.8[209] | K1.5IIIFe-0.5 | |
| π1 Gruis | 21[210] | ? | 535[210] | S5,7 | |
| Aldebaran (α Tauri) |
20.58[211]–21.1[212] | LD | 65.3±1[213] | K5+III | |
| GY Aquilae | 20.46[24] | ? | 1108±98[24] | M8 | |
| θ Apodis | 18.1[214] | ? | 389±17[215] | M6.5III | |
| R Lyrae | 18.016±0.224[212] | LD | 310+10−7[216] | M4.5III | |
| Scheat (β Pegasi) |
16.75±0.24[217] | Ross | 196±2[206] | M2.5II-III | |
| Gorgonea Tertia (ρ Persei) |
16.555±0.166[212] | LD | 308±7[206] | M4+IIIa | |
| SW Virginis | 16.11±0.13–16.8±0.34[218] | UD | 527±46.9[219] | M7III: | |
| R Aquarii | 15.61±0.8 – 16.59±1.03[218] | LD | 711+39−36[220] | M6.5–M8.5e | |
| g Herculis | 15.2±0.5 – 19.09±0.19[218] | LD | 385±10[216] | M6-III | |
| RS Cancri | 15.1±0.5 – 17.2±0.4[212] | LD | 490±40[221] | M6S | |
| Tejat (μ Geminorum) |
15.118±0.151[212] | LD | 230±10[206] | M3IIIab | |
| R Leonis Minoris | 14.4±0.87[218] | LD | 942+33−47[216] | M6.5-9e | |
| S Cephei | 14.29±2.28[218] | LD | 1591+49−46[216] | C7,3e | |
| T Cassiopeiae | 14.22±0.73[218] | LD | 893+49−46[216] | M7-9e | |
| μ Cephei (Herschel's Garnet Star) | 14.11 ± 0.6[46] | 2,000[45]–3060+460−130[44] | M2Ia | ||
| Mirach (β Andromedae) |
13.749±0.137[212] | LD | 199±9[222] | M0+IIIa | |
| Menkar (α Ceti) |
13.238±0.056[212] | LD | 249±8[206] | M1.5IIIa | Other measurements include 12.2±0.04 mas.[223] |
| V Cygni | 13.1±0.208 – 14.84±2.37[218] | LD | 1747+163−137[216] | C7,4eJ |
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
- ↑ 1.0 1.1 1.2 1.3 1.4 1.5 Methods for calculating the radius:
- AD: radius calculated from angular diameter and distance
- L/Teff: radius calculated from bolometric luminosity and effective temperature
- SEIS: radius obtained from seismic data
- OD: radius obtained from optical depth
- ↑ 2.0 2.1 2.2 2.3 2.4 2.5 At the J2000 epoch
- ↑ Using an angular diameter of 7.8±0.64 milliarcseconds[38] and a distance of 1610+130
−110 parsecs.[33] - ↑ Luminosities are calculated using the apparent bolometric magnitude and distances in the following equation:
100.4
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- ↑ Calculated using a distance of 432 parsecs and an angular diameter of 2.31 milliarcseconds.
- ↑ Legend:
UD=Uniform disk diameter
LD=Limb-darkened diameter
Ross=Rosseland diameter
Est = Estimated using distance and physical radius
References
- ↑ Mamajek, E. E.; Prsa, A.; Torres, G.; Harmanec, P.; Asplund, M.; Bennett, P. D.; Capitaine, N.; Christensen-Dalsgaard, J.; Depagne, E.; Folkner, W. M.; Haberreiter, M. (October 2015). "IAU 2015 Resolution B3 on Recommended Nominal Conversion Constants for Selected Solar and Planetary Properties". arXiv:1510.07674 [astro-ph.SR].
- ↑ Rau, A.; Kulkarni, S. R.; Ofek, E. O.; Yan, L. (2007). "Spitzer Observations of the New Luminous Red Nova M85 OT2006-1". The Astrophysical Journal 659 (2): 1536–1540. doi:10.1086/512672. Bibcode: 2007ApJ...659.1536R.
- ↑ Haemmerlé, Lionel; Woods, T. E.; Klessen, Ralf S.; Heger, Alexander; Whalen, Daniel J. (2018). "The evolution of supermassive Population III stars". Monthly Notices of the Royal Astronomical Society 474 (2): 2757–2773. doi:10.1093/mnras/stx2919.
- ↑ Herrington, Nicholas P.; Whalen, Daniel J.; Woods, Tyrone E. (2023). "Modelling supermassive primordial stars with <SCP>mesa</SCP>". Monthly Notices of the Royal Astronomical Society 521: 463–473. doi:10.1093/mnras/stad572.
- ↑ Haemmerlé, L.; Klessen, R. S.; Mayer, L.; Zwick, L. (2021). "Maximum accretion rate of supermassive stars". Astronomy & Astrophysics 652: L7. doi:10.1051/0004-6361/202141376. Bibcode: 2021A&A...652L...7H.
- ↑ Gray, David F. (1967-08-01). "Photometric Determination of Stellar Radii". The Astrophysical Journal 149: 317. doi:10.1086/149256. ISSN 0004-637X. Bibcode: 1967ApJ...149..317G.
- ↑ Meyer, C.; Rabbia, Y.; Froeschle, M.; Helmer, G.; Amieux, G. (1995-04-01). "Observations of lunar occultations at Observatoire de la Cote d'Azur". Astronomy and Astrophysics Supplement Series 110: 107. ISSN 0365-0138. Bibcode: 1995A&AS..110..107M.
- ↑ Levesque, Emily M.; Massey, Philip; Olsen, K. A. G.; Plez, Bertrand; Meynet, Georges; Maeder, Andre (July 2006). "The Effective Temperatures and Physical Properties of Magellanic Cloud Red Supergiants: The Effects of Metallicity". The Astrophysical Journal 645 (2): 1102–1117. doi:10.1086/504417. ISSN 0004-637X. Bibcode: 2006ApJ...645.1102L.
- ↑ Ren, Yi; Jiang, Bi-Wei (July 2020). "On the Granulation and Irregular Variation of Red Supergiants". The Astrophysical Journal 898 (1): 24. doi:10.3847/1538-4357/ab9c17. ISSN 0004-637X. Bibcode: 2020ApJ...898...24R.
- ↑ 10.0 10.1 10.2 10.3 10.4 10.5 "HORIZONS Web-Interface". https://ssd.jpl.nasa.gov/horizons.cgi.
- ↑ 11.0 11.1 11.2 11.3 11.4 Healy, Sarah; Horiuchi, Shunsaku; Ashall, Chris (5 December 2024). "The Red Supergiant Problem: As Seen from the Local Group's Red Supergiant Populations". arXiv:2412.04386 [astro-ph.SR].
- ↑ 12.0 12.1 12.2 12.3 12.4 12.5 Levesque, Emily M.; Massey, Philip; Plez, Bertrand; Olsen, Knut A. G. (2009). "The Physical Properties of the Red Supergiant WOH G64: The Largest Star Known?". The Astronomical Journal 137 (6): 4744. doi:10.1088/0004-6256/137/6/4744. Bibcode: 2009AJ....137.4744L.
- ↑ 13.00 13.01 13.02 13.03 13.04 13.05 13.06 13.07 13.08 13.09 13.10 de Wit, S.; Bonanos, A.Z.; Tramper, F.; Yang, M.; Maravelias, G.; Boutsia, K.; Britavskiy, N.; Zapartas, E. (2023). "Properties of luminous red supergiant stars in the Magellanic Clouds". Astronomy and Astrophysics 669: 17. doi:10.1051/0004-6361/202243394. Bibcode: 2023A&A...669A..86D.
- ↑ 14.0 14.1 14.2 14.3 Levesque, E. M. (June 2010). "The Physical Properties of Red Supergiants". Hot and Cool: Bridging Gaps in Massive Star Evolution ASP Conference Series. 425. p. 103. Bibcode: 2010ASPC..425..103L.
- ↑ 15.0 15.1 15.2 15.3 15.4 15.5 15.6 15.7 Beasor, Emma R.; Smith, Nathan (2022-05-01). "The Extreme Scarcity of Dust-enshrouded Red Supergiants: Consequences for Producing Stripped Stars via Winds". The Astrophysical Journal 933 (1): 41. doi:10.3847/1538-4357/ac6dcf. Bibcode: 2022ApJ...933...41B.
- ↑ 16.0 16.1 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. doi:10.1093/mnras/stw2708. Bibcode: 2017MNRAS.465..403G.
- ↑ 17.0 17.1 Jones, Olivia; Woods, Paul; Kemper, Franziska; Kraemer, Elena; Sloan, G.; Srinivasan, Sivakrishnan; Oliveira, Joana; van Loon, Jacco et al. (May 7, 2017). "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. doi:10.1093/mnras/stx1101.
- ↑ 18.00 18.01 18.02 18.03 18.04 18.05 18.06 18.07 18.08 18.09 18.10 18.11 18.12 18.13 18.14 18.15 18.16 18.17 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. doi:10.3847/1538-3881/abab15. Bibcode: 2020AJ....160..145H.
- ↑ 19.0 19.1 Wittkowski, M.; Hauschildt, P. H.; Arroyo-Torres, B.; Marcaide, J. M. (April 2012). "Fundamental properties and atmospheric structure of the red supergiant VY Canis Majoris based on VLTI/AMBER spectro-interferometry". Astronomy and Astrophysics 540: L12. doi:10.1051/0004-6361/201219126. ISSN 0004-6361. Bibcode: 2012A&A...540L..12W.
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- ↑ Gordon, Michael S.; Jones, Terry J.; Humphreys, Roberta M.; Ertel, Steve; Hinz, Philip M.; Hoffman, William F.; Stone, Jordan; Spalding, Eckhart et al. (February 2019). "Thermal Emission in the Southwest Clump of VY CMa". The Astronomical Journal 157 (2): 57. doi:10.3847/1538-3881/aaf5cb. Bibcode: 2019AJ....157...57G.
- ↑ Nguyen, Thinh H.; Guinan, Edward F. (2022-01-11). "Stars on the Verge: Analyses of the Complex Light Variations of the Hyper-luminous Red Supergiant VY Canis Majoris: On the Nature of the Star's "Great Dimming" Episodes". Research Notes of the AAS 6 (1): 12. doi:10.3847/2515-5172/ac4991. ISSN 2515-5172. Bibcode: 2022RNAAS...6...12N.
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- ↑ González-Torà, G.; Wittkowski, M.; Davies, B.; Plez, B. (December 19, 2023). "The effect of winds on atmospheric layers of red supergiants II. Modelling VLTI/GRAVITY and MATISSE observations of AH Sco, KW Sgr, V602 Car, CK Car and V460 Car". Astronomy & Astrophysics 683: A19. doi:10.1051/0004-6361/202348047. ISSN 0004-6361. Bibcode: 2024A&A...683A..19G.
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- ↑ Xu, Shuangjing; Zhang, Bo; Reid, Mark J; Menten, Karl M; Zheng, Xingwu; Wang, Guangli (2018). "The Parallax of the Red Hypergiant VX Sgr with Accurate Tropospheric Delay Calibration". The Astrophysical Journal 859 (1): 14. doi:10.3847/1538-4357/aabba6. Bibcode: 2018ApJ...859...14X.
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- ↑ Fok, Thomas K. T.; Nakashima, Jun-ichi; Yung, Bosco H. K.; Hsia, Chih-Hao; Deguchi, Shuji (November 2012). "Maser Observations of Westerlund 1 and Comprehensive Considerations on Maser Properties of Red Supergiants Associated with Massive Clusters". The Astrophysical Journal 760 (1): 65. doi:10.1088/0004-637X/760/1/65. ISSN 0004-637X. Bibcode: 2012ApJ...760...65F.
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- ↑ Min, Cheulhong; Matsumoto, Naoko; Kim, Mi Kyoung; Hirota, Tomoya; Shibata, Katsunori M.; Cho, Se-Hyung; Shizugami, Makoto; Honma, Mareki (2014-04-01). "Accurate Parallax Measurement toward the Symbiotic Star R Aquarii". Publications of the Astronomical Society of Japan 66 (2): 38. doi:10.1093/pasj/psu003. ISSN 2053-051X.
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- ↑ "HD 6860 Overview". NASA Exoplanet Archive. https://exoplanetarchive.ipac.caltech.edu/overview/HD%206860.
- ↑ Wittkowski, M. et al. (December 2006), "Tests of stellar model atmospheres by optical interferometry. IV. VINCI interferometry and UVES spectroscopy of Menkar", Astronomy and Astrophysics 460 (3): 855–864, doi:10.1051/0004-6361:20066032, Bibcode: 2006A&A...460..855W
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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
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