List of largest stars should not be confused with List of most massive stars.
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 1solar radius).
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.
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, comparable to some of the largest known black holes.
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 supergiants can be occulted by the Moon, including Antares and 119 Tauri. 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.
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:
The following lists show the largest known stars based on the host galaxy.
| Star name | Solar radius | Method | Notes< | --
See template documentation (Template:List of largest stars row) for more information about formatting/inputThe table break | - does not need to be placed between template calls, but needs to be placed before manually-inserted linesEvery number/pair of numbers must have a reference!--> |
|---|---|---|---|---|---|
| Orbit of Saturn | – | Reported for reference | |||
| Theoretical limit of star size (Milky Way) | ~–1,800 | 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. Higher value is derived from evolutionary modelling of red supergiants with low metallicites and an initial mass of . Reported for reference | |||
| RSGC1-F01 | L/Teff | ||||
| VY Canis Majoris | 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. Potentially the largest known star in the Milky Way. There is a possilbility that this size might be a bit overestimated (on the order of 1 sigma). Hence, the quoted radius might be just an upper limit. | |||
| AH Scorpii | AD | ||||
| RSGC1-F06 | L/Teff | ||||
| S Persei | AD | ||||
| VX Sagittarii | 1,356 – | AD | The most luminous known asymptotic giant branch star. Widely recognised as being among the largest known stars. | ||
| NML Cygni | < | AD | Surrounding dusty region is very complex making the radius hard to determine. | ||
| Stephenson 2 DFK 2 | L/Teff | Another red supergiant, Stephenson 2 DFK 1 has an estimated radius of . However, it is potentially not a member of the Stephenson 2 cluster and also has a distance with an uncertainty of ≳50% due to it only being measured with radial velocities. | |||
| Stephenson 2 DFK 49 | L/Teff | A K-type star similar to the yellow hypergiant IRC +10420 that has left its red supergiant stage. | |||
| HD 143183 (V558 Normae) | 1,261 | L/Teff | |||
| PZ Cassiopeiae | , | L/Teff & AD | |||
| μ Cephei (Herschel's Garnet Star) | 1,259, 1,420, | L/Teff & AD | Widely recognised as being among the largest known stars. Might be the largest star visible to the naked eye.[1] | ||
| RSGC1-F10 | L/Teff | ||||
| V354 Cephei | 1,245 | L/Teff | |||
| Westerlund 1 W237 (Westerlund 1 BKS B) | L/Teff | ||||
| ST Cephei | 1,218 | L/Teff | |||
| IRC -10414 | ~ | L/Teff | |||
| V517 Monocerotis | L/Teff | ||||
| RSGC1-F05 | L/Teff | ||||
| GCIRS 7 | ,, | AD & L/Teff | |||
| Westerlund 1 W26 (Westerlund 1 BKS AS) | – | L/Teff | |||
| [A72c] 16 | 1,157 | L/Teff | |||
| WY Velorum A | 1,157 | L/Teff | A symbiotic binary. | ||
| RSGC1-F08 | L/Teff | ||||
| RSGC1-F02 | L/Teff | ||||
| Orbit of Jupiter | – | Reported for reference | |||
| V582 Cassiopeiae | 1,111 | L/Teff | |||
| RW Cygni | AD | ||||
| RW Cephei | AD | A K-type hypergiant star that experienced a "great dimming" event in 2022, similar to Betelgeuse. | |||
| RT Carinae | 1,090 | L/Teff | |||
| RSGC1-F04 | , 1,100, | L/Teff | |||
| UU Persei | L/Teff | ||||
| LL Pegasi | 1,074 | L/Teff | |||
| HD 126577 | L/Teff | ||||
| V766 Centauri Aa | 1,060–1,160 | ? | V766 Centauri Aa is a rare variable yellow hypergiant. | ||
| CM Velorum | 1,048 | L/Teff | |||
| AG Camelopardalis | 1,048 | L/Teff | |||
| , | AD | ||||
| AD | |||||
| RSGC1-F11 | L/Teff | ||||
| BC Cygni | 1,031– | L/Teff | A more detailed but older study gives values of (–) for the year 2000, and (–) for the year 1900. | ||
| MY Cephei | L/Teff | ||||
| V530 Cassiopeiae | 1,017 | L/Teff | |||
| RSGC1-F13 | L/Teff | ||||
| V602 Carinae | 1,015 | AD | |||
| VV Cephei A | 1,015 | AD | A red supergiant star orbited by a smaller B-type main-sequence star with a radius estimated between 13 and . Widely recognised as being among the largest known stars. Another estimate give a radius of based on the Gaia DR3 distance of 1 kpc. | ||
| U Lacertae A | 1,013 | L/Teff | |||
| KW Sagittarii | AD | ||||
| Ve 4-64 | 1,007 | L/Teff | |||
| RSGC1-F07 | L/Teff | ||||
| V349 Carinae | L/Teff | ||||
| V674 Cephei | 999 | L/Teff | |||
| RSGC1-F09 | L/Teff | ||||
| IRAS 18111-2257 | ~ | 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 . | ||
| CIT 11 | 982 | L/Teff | |||
| V381 Cephei Aa | 977 | L/Teff | |||
| MSX6C G086.5890–00.7718 | (–)– | 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 | L/Teff | |||
| 964 | L/Teff | ||||
| RSGC1-F12 | L/Teff | ||||
| RSGC1-F03 | L/Teff | ||||
| V398 Cassiopeiae (HD 240275) | 941 | L/Teff | |||
| IRC +60342 | 940 | L/Teff | |||
| ψ1 Aurigae | 934 | L/Teff | |||
| V645 Cephei | 920 | L/Teff | |||
| UY Scuti | L/Teff | Initially reported, making it the largest star, a 2023 measurement put the radius at a smaller value of based on the multimessenger monitoring of supernovae. | |||
| NR Vulpeculae | 908 | L/Teff | |||
| KU Andromedae (IRC +40004) | L/Teff | ||||
| V774 Sagittarii | 889 | L/Teff | |||
| V923 Centauri | 881 | L/Teff | |||
| IRAS 20341+4047 | 880 | L/Teff | |||
| V540 Sagittarii | 880 | L/Teff | |||
| V386 Cephei | 879 | L/Teff | |||
| Trumpler 27-1 (CD-33 12241) | ? | ||||
| TYC 3996-552-2 | 870 | L/Teff | |||
| V1300 Aquilae (IRC −10529) | – | L/Teff | |||
| Westerlund 1 W20 (Westerlund 1 BKS D) | L/Teff | ||||
| AZ Cygni | AD | Estimated based on data from the CHARA array. Another radii of (2014), (2015) and (2016) are calculated based on the same data. | |||
| V348 Velorum | 855 | L/Teff | |||
| BI Cygni | AD | ||||
| TW Carinae | 835 | L/Teff | |||
| V358 Cassiopeiae | 835 | L/Teff | |||
| DO 26226 | 826 | L/Teff | |||
| HD 155737 | 823 | L/Teff | |||
| 6 Geminorum | 821 | L/Teff | |||
| RW Leonis Minoris | L/Teff | ||||
| HD 300933 | 806 | L/Teff | |||
| [W61c] R 53 | 801 | L/Teff | |||
| U Arietis | AD | ||||
| RT Ophiuchi | AD | ||||
| HD 95687 | 797 | L/Teff | |||
| BO Carinae | L/Teff | ||||
| HD 62745 | 790 | L/Teff | |||
| WX Piscium | [2] | L/Teff | |||
| VR5–7 | L/Teff | ||||
| V Cygni | L/Teff | ||||
| CL Carinae | 770 | L/Teff | |||
| RS Persei | , | AD | |||
| V355 Cephei | 790 | L/Teff | |||
| BD+63 3 | 770 | L/Teff | |||
| BD+63 270 | 769 | L/Teff | |||
| V644 Cephei | 765 | L/Teff | |||
| BM VIII 11 | 754 | L/Teff | |||
| [SLN74] 2130 | 752 | L/Teff | |||
| IRAS 10176-5802 | –(–) | 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 | L/Teff | ||||
| R Leporis (Hind's Crimson Star) | 750[3] | AD | Size range from 645 to 860 . | ||
| V384 Persei | L/Teff | ||||
| GY Aquilae | AD | ||||
| UU Pegasi | AD | ||||
| IM Cassiopeiae | 740 | L/Teff | |||
| Stephenson 2 DFK 10 | 730 | L/Teff | |||
| HD 105563 A | 723 | L/Teff | |||
| Westerlund 1 W75 (Westerlund 1 BKS E) | L/Teff | ||||
| V1111 Ophiuchi (IRC +10365) | L/Teff | ||||
| XX Persei | AD | Another study from the same author estimates . | |||
| 716 | L/Teff | ||||
| V Camelopardalis | AD | ||||
| CD-61 3575 | 716 | L/Teff | |||
| AS Cephei | 713 | L/Teff | |||
| V770 Cassiopeiae (BD+60 299) | 713 | L/Teff | |||
| 712 | L/Teff | ||||
| MZ Puppis | 708 | L/Teff | |||
| GP Cassiopeiae | 707 | L/Teff | |||
| GCIRS 12N | L/Teff | ||||
| V528 Carinae | L/Teff | ||||
| The following well-known stars are listed for the purpose of comparison. | |||||
| Antares (α Scorpii A) | AD | Fourteenth brightest star in the night sky. Widely recognised as being among the largest known stars. | |||
| Betelgeuse (α Orionis) | 640,, 782 ± 55[4] | AD & SEIS | Tenth brightest star in the night sky. Widely recognised as being among the largest known stars, radius decreased to during the 2020 great dimming event. | ||
| R Horologii | 635 | 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. | ||
| 119 Tauri (CE Tauri, Ruby Star) | 587593 | AD | |||
| ρ Cassiopeiae | AD | A yellow hypergiant star, similar to V382 Carinae, that is also visble to the naked eye. | |||
| CW Leonis | 560 | L/Teff | The nearest carbon star. | ||
| V509 Cassiopeiae | AD | A variable yellow hypergiant whose size varied from around in 1950–1970 to in 1977, and later decreased to in the 1990s. | |||
| V838 Monocerotis | 464 | L/Teff | During the 2002 Red Nova, the star's radius may have increased up to . | ||
| Pistol Star (V4647 Sagittarii) | L/Teff | One of the most luminous stars known. | |||
| Mira (ο Ceti A) | 332–402 | AD | Prototype of the Mira variables. | ||
| Orbit of Mars | – | Reported for reference | |||
| R Doradus | AD | The extrasolar star with the largest apparent size. | |||
| Rasalgethi (α Herculis A) | (–) | L/Teff | |||
| Cygnus OB2#12 | 246 | ? | One of the most massive and luminous stars known. | ||
| Orbit of Earth (~1 AU) | Reported for reference | ||||
| Suhail (λ Velorum) | AD | ||||
| Wezen (δ Canis Majoris) | 188 | L/T | Thirty-sixth brightest star in the night sky. | ||
| Enif (ε Pegasi) | 178 | L/Teff | |||
| Orbit of Venus | Reported for reference | ||||
| η Carinae A | 128742 | OD | During the 1843 Great Eruption, the star's radius may have increased up to 4,319–6,032 . | ||
| Deneb (α Cygni) | AD & ? | Eighteenth brightest star in the night sky. | |||
| Orbit of Mercury | – | Reported for reference | |||
| Rigel (β Orionis A) | AD | Seventh brightest star in the night sky. | |||
| Canopus (α Carinae) | 73.3 | AD | Second brightest star in the night sky. | ||
| Gacrux (γ Crucis) | 73 | L/Teff | |||
| Polaris (α Ursae Minoris) | AD | The current star in the North Pole. It is a Classical Cepheid variable, and the brightest example of its class. | |||
| Aldebaran (α Tauri) | AD | Fourteenth brightest star in the night sky. | |||
| Arcturus (α Boötis) | 25.4 ± 0.2 | 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 | AD | The nearest giant star to the Earth. | ||
| Spica (α Virginis A) | One of the nearest supernova candidates and the sixteenth-brightest star in the night sky. | ||||
| Regulus (α Leonis A) | 4.16 × 3.14 | The nearest B-type star to the Earth. | |||
| Vega (α Lyrae) | × | AD | Fifth brightest star in the night sky. | ||
| Altair (α Aquilae) | 2.01 × 1.57 | Twelfth brightest star in the night sky. | |||
| Sirius (α Canis Majoris A) | 1.713[5] | AD | The brightest star in the night sky. | ||
| Rigil Kentaurus (α Centauri A) | 1.2175 | AD | Third brightest star in the night sky. | ||
| Sun | The largest object in the Solar System. | ||||
| Solar radii (Sun = 1) | Galaxy | Method | Notes | ||
|---|---|---|---|---|---|
| HV 888 | 1,477[6] –1,584 | Large Magellanic Cloud | L/Teff | ||
| IRAS 05280–6910 | 1,367 | Large Magellanic Cloud | L/Teff | The most reddened object in the Large Magellanic Cloud. | |
| IRAS 05346-6949 | 1,211 | Large Magellanic Cloud | L/Teff | It has an estimated mass-loss rate of 0.0017 (566 Earths) per year, the highest for any star. | |
| HV 2242 | 1,160 | Large Magellanic Cloud | L/Teff | ||
| MSX SMC 018 | 1,119 | Small Magellanic Cloud | L/Teff | ||
| WOH S338 | 1,100 | Large Magellanic Cloud | L/Teff | ||
| IRAS 04516-6902 | 1,085 | Large Magellanic Cloud | L/Teff | ||
| MSX LMC 589 | 1,051 | Large Magellanic Cloud | L/Teff | ||
| IRAS 05402-6956 | 1,032 | Large Magellanic Cloud | L/Teff | ||
| 1,027–1,187 | Large Magellanic Cloud | L/Teff | |||
| B90 (WOH S264) | 1,210 | Large Magellanic Cloud | L/Teff | Has an unusually high metallicity and velocity. Often referred to as its SIMBAD designation [W60] B90. Discrepancy in radius is caused by a potential underestimation of the effective temperature measured from the Titanium(II) oxide bands. | |
| HV 2450 | –1,071 | Large Magellanic Cloud | L/Teff | A yellow hypergiant. | |
| UCAC2 2674864 (HV 2834) | Large Magellanic Cloud | L/Teff | |||
| HV 2362 | 1,030 | Large Magellanic Cloud | L/Teff | ||
| MG73 59 | 979 | Large Magellanic Cloud | L/Teff | A yellow supergiant. | |
| HD 268757 | 979 | Large Magellanic Cloud | L/Teff | A G8 yellow hypergiant. | |
| LMC 147199 | 990 | Large Magellanic Cloud | L/Teff | ||
| LMC 23095 | 926 – 1,280 | Large Magellanic Cloud | L/Teff | ||
| SP77 31-16 | Large Magellanic Cloud | L/Teff | A yellow hypergiant. | ||
| LMC 66778 | 990 | Large Magellanic Cloud | L/Teff | ||
| WOH S457 | Large Magellanic Cloud | L/Teff | |||
| IRAS 04498-6842 (LI-LMC 60) | 898, | 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 . | |
| HV 12185 | Large Magellanic Cloud | L/Teff | |||
| HV 12793 | Large Magellanic Cloud | L/Teff | |||
| WOH S57 | Large Magellanic Cloud | L/Teff | |||
| SP77 28-2 | Large Magellanic Cloud | L/Teff | |||
| SP77 22-9 | 850 | Large Magellanic Cloud | L/Teff | ||
| Z Doradus | –956 | Large Magellanic Cloud | L/Teff | ||
| WOH G64 | ~800[7] | Large Magellanic Cloud | L/Teff | Surrounded by a large torus-shaped dust envelope. Transitioned from a red supergiant into a yellow hypergiant after a potential 30 year long outburst. Previously estimated to be | |
| SP77 40-7 | 810 | Large Magellanic Cloud | L/Teff | ||
| W61 19–24 | Large Magellanic Cloud | L/Teff | |||
| WOH S28 | 780 | Large Magellanic Cloud | L/Teff | ||
| SP77 48-6 | 768 | Large Magellanic Cloud | L/Teff | ||
| WOH S452 | Large Magellanic Cloud | L/Teff | |||
| WOH S438 | Large Magellanic Cloud | L/Teff | |||
| LMC 139027 | 790 | Large Magellanic Cloud | L/Teff | ||
| SP77 45-16 | 800 | Large Magellanic Cloud | L/Teff | ||
| SP77 54-27 | 750800 | Large Magellanic Cloud | L/Teff | ||
| SP77 39-17 | 760 | Large Magellanic Cloud | L/Teff | ||
| HD 269723 | , 814–829 | Large Magellanic Cloud | L/Teff | A yellow hypergiant. | |
| PMMR 64 | Small Magellanic Cloud | L/Teff | |||
| LH 43-15 | 740 | Large Magellanic Cloud | L/Teff | ||
| PMMR 116 | 717 | Small Magellanic Cloud | L/Teff | ||
| MSX SMC 055 | 702– | Small Magellanic Cloud | L/Teff | A super-AGB candidate. | |
| SP77 48-6 | 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 | Small Magellanic Cloud | L/Teff | It has been previously considered to be a possible Thorne–Żytkow object. | |
| HV 11417 | 673–798 | Small Magellanic Cloud | L/Teff | Candidate Thorne-Zytkow object. | |
| HD 269953 | 647–720 | Large Magellanic Cloud | L/Teff | A yellow hypergiant. | |
| HD 33579 | 471 | Large Magellanic Cloud | L/Teff | The brightest star in the Large Magellanic Cloud. | |
| S Doradus | 100 | Large Magellanic Cloud | L/Teff | A luminous blue variable in the S Doradus instability strip. | |
| HD 37974 | 99 | Large Magellanic Cloud | L/Teff | An unusual blue hypergiant with a large dusty disk. | |
| R136a1 | Large Magellanic Cloud | L/Teff | One of the most luminous and most massive stars. | ||
| BAT 99-98 | 37.5 | Large Magellanic Cloud | L/Teff | One of the most luminous and most massive stars. | |
| HD 5980 A | 24 | Small Magellanic Cloud | L/Teff | A luminous blue variable and one of the most luminous stars. | |
| Star name | Solar radii (Sun = 1) | Galaxy | Method | Notes | |
|---|---|---|---|---|---|
| LGGS J004428.48+415130.9 | 1,410 | Andromeda Galaxy | L/Teff | ||
| LGGS J013418.56+303808.6 | 1,363 | Triangulum Galaxy | L/Teff | ||
| LGGS J004255.95+404857.5 | 785 | Andromeda Galaxy | L/Teff | ||
| LGGS J004124.80+411634.7 | 760, 1,205, 1,240 | Andromeda Galaxy | L/Teff | ||
| LGGS J013349.86+303246.1 | 710–795 | Triangulum Galaxy | L/Teff | A yellow supergiant. | |
| The following well-known stars are listed for the purpose of comparison. | |||||
| Var 83 | 150 | Triangulum Galaxy | L/Teff | A luminous blue variable and one of the most luminous stars in M33. | |
| Star name | Solar radii (Sun = 1) | Galaxy | Method | Notes< | --
See template documentation (Template:List of largest stars row) for more information about formatting/inputThe table break | - does not need to be placed between template calls, but needs to be placed before manually-inserted linesEvery number/pair of numbers must have a reference!--> |
|---|---|---|---|---|---|---|
| Sextans A 10 | Sextans A | L/Teff | ||||
| NGC 6822-RSG 19 | 930[8] | NGC 6822 | L/Teff | |||
| WLM 02 | WLM | L/Teff | ||||
| Sextans A 5 | Sextans A | L/Teff | ||||
| NGC 6822-RSG 26 | 868[9] | NGC 6822 | L/Teff | |||
| NGC 6822-RSG 12 | 839[10] | NGC 6822 | L/Teff | |||
| NGC 6822-RSG 9 | 765[11] | NGC 6822 | L/Teff | |||
| NGC 6822-RSG 6 | 714[12] | NGC 6822 | L/Teff | |||
| Sextans A 7 | Sextans A | L/Teff | ||||
| The following well-known stars are listed for the purpose of comparison. | ||||||
| NGC 6822-WR 12 | 3.79 | NGC 6822 | L/Teff | A Wolf-Rayet star, one of the hottest known stars. | ||
| Star name | Solar radii (Sun = 1) | Galaxy | Group | Method | Notes< | --
See template documentation (Template:List of largest stars row) for more information about formatting/inputThe table break | - does not need to be placed between template calls, but needs to be placed before manually-inserted linesEvery number/pair of numbers must have a reference!--> |
|---|---|---|---|---|---|---|---|
| NGC 1313-310 | NGC 1313 | L/Teff | Luminosity has not yet been constrained well enough yet to confirm its extreme properties, and further observations are needed to show that it is a single, uncontaminated star. Effective temperature is based on Titanium(II) oxide lines, which often results in lower values, therefore increasing the radius. | ||||
| NGC 300-125 | 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. | |||
| NGC 247-154 | 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. | |||
| NGC 7793-34 | 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. | |||
| NGC 55-40 | 1,286 | 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. | ||
| NGC 300-154 | 1,200 | 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. | ||
| NGC 300-114 | 1,181 | 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. | ||
| NGC 300-199 | 1,181 | 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. | ||
| NGC 300-153 | 1,173 | 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. | ||
| NGC 300-150 | 1,167 | 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. | ||
| NGC 253-2006 | 1,167 | 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. | ||
| SPIRITS 14atl | 1,134–1,477 | Messier 83 | Centaurus A/M83 Group | L/Teff | |||
| NGC 300-59 | 1,133 | 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. | ||
| NGC 7793-86 | 1,127 | 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. | ||
| NGC 300-263 | 1,108 | 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. | ||
| NGC 247-447 | 1,101 | 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. | ||
| SPIRITS 15ahp | 1,098 | NGC 2403 | M81 Group | L/Teff | |||
| NGC 300-240 | 1,088 | 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. | ||
| NGC 7793-86 | 1,078 | 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. | ||
| NGC 300-173 | 1,063 | 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. | ||
| NGC 300-340 | 1,036 | 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. | ||
| NGC 300-346 | 1,023 | 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. | ||
| NGC 247-533 | 1,004 | 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. | ||
| NGC 300-351 | 992 | 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. | ||
| NGC 300-524 | 987 | 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. | ||
| NGC 55-135 | 964 | 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. | ||
| NGC 55-93 | 955 | 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. | ||
| NGC 7793-539 | 948 | 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. | ||
| NGC 55-87 | 948 | 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. | ||
| NGC 55-146 | 921 | 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. | ||
| NGC 300-273 | 921 | 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. | ||
| NGC 300-186 | 915 | 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. | ||
| NGC 55-200 | 905 | 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. | ||
| NGC 55-152 | 895 | 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. | ||
| NGC 300-413 | 861 | 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. | ||
| NGC 55-174 | 856 | 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. | ||
| NGC 55-75 | 836 | 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. | ||
| NGC 300-545 | 824 | 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. | ||
| NGC 247-2912 | 821 | 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. | ||
| NGC 55-216 | 801 | 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. | ||
| NGC 247-1471 | 798 | 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. | ||
| NGC 300-499 | 796 | 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. | ||
| NGC 300-379 | 744 | 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. | ||
| NGC 300-838 | 744 | 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. | ||
| NGC 55-149 | 738 | 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. | ||
| NGC 55-194 | 730 | 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. | ||
| NGC 55-270 | 728 | 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. | ||
| NGC 300-1047 | 724 | 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. | ||
| NGC 247-3231 | 719 | 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. | ||
| NGC 247-2966 | 719 | 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. | ||
| NGC 55-245 | 717 | 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. | ||
| NGC 300-1068 | 716 | 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. | ||
| NGC 300-1081 | 712 | 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. | ||
| The following well-known stars are listed for the purpose of comparison. | |||||||
| NGC 2363-V1 | – | NGC 2366 | M81 Group | L/Teff | |||
Note that this list does not include the candidate JWST dark stars, with estimated radii of up to 61au or Quasi-stars, with theoretical models suggesting that they could reach radii of up to 40700solar radius.
During some transient events, such as red novae or LBV eruptions the star's radius can increase by a significant amount.
| AT 2017jfs | 33,000 | 2017 | NGC 4470 | L/Teff | |||
| SNhunt151 | 2014 | UGC 3165 | LDC 331 | L/Teff | |||
| SN 2015bh | 2015 | NGC 2770 | LDC 616 | L/Teff | |||
| AT 2018hso | 10,350 | 2018 | NGC 3729 | M109 Group | L/Teff | ||
| AT 2023clx | 2023 | NGC 3799 | nest 101314 | L/Teff | |||
| M51 OT2019-1 | 2019 | Whirlpool Galaxy | M51 Group | L/Teff | |||
| η Carinae | 4,319 – 6,032 | 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. | |
| AT 2010dn | 2010 | NGC 3180 | LDC 743 | L/Teff | |||
| SN 2011fh | 3,980 | 2011 | NGC 4806 | Abell 3528 | L/Teff | ||
| AT 2014ej | 2014 | NGC 7552 | Grus Quartet | L/Teff | |||
| V838 Monocerotis | 3,190 | 2002 | Milky Way | Local Group | L/Teff | ||
| SN2008S | 2008 | NGC 6946 | NGC 6946 Group | L/Teff | |||
| SNhunt120 | 2012 | NGC 5775 | Virgo Cluster | L/Teff | |||
| AT 2017be | 2017 | NGC 2537 | L/Teff | ||||
| PHL 293B star | 1,348 – 1,463 | 2002 | PHL 293B | L/Teff | |||
| SNhunt248 | ~850 | 2014 | NGC 5806 | NGC 5846 Group | L/Teff | ||
| R71 | 500 | 2012 | Large Magellanic Cloud | Local Group | L/Teff | ||
| SN 2000ch | 500 | 2000 | NGC 3432 | LDC 743 | L/Teff | ||
| Godzilla | 430 – 2,365 | 2015 | Sunburst galaxy | ? | |||
| AT 2016blu | ~330 | 20122022 | 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 19992009. |
| SN 2020faa | 2020 | 2MASS J14470904+7244157 | L/Teff | ||||
| SN 2023ixf | – | 2023 | Pinwheel galaxy | M101 Group | L/Teff | ||
| SN 2020jfo | 2020 | Messier 61 | Virgo Cluster | L/Teff | |||
| SN 2023axu | 2023 | NGC 2283 | L/Teff | ||||
| SN 2021agco | 2021 | UGC 3855 | LDC 506 | L/Teff | Nearest ultrastripped supernova known. |
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 . Stars with angular diameters larger than 13milliarcseconds are included.
| Sun | 2,000,000 | 0.000016 | G2V | angular diameter. | ||
| R Doradus | 51.18 | LD | 179 | M8III:e | angular diameter apart from the Sun. | |
| Betelgeuse (α Orionis) | 42.28 | LD | 408–540 | |||
| Antares (α Scorpii A) | 37.31 | LD | 553.5 | M1.5Iab | ||
| Mira (ο Ceti) | 28.934.9 | Ross | 299 | M5-M9IIIe | The angular diameter vary during Mira's pulsations. | |
| Gacrux (γ Crucis) | 24.7 | ? | 88.6 | M3.5III | ||
| Rasalgethi (α Herculis) | 23.95 | Est | 359 | M5Ib-II | ||
| R Hydrae | 23.7 | ? | 482 | M6-9e | ||
| Arcturus (α Boötis) | 21.06 | LD | 36.8 | K1.5IIIFe-0.5 | ||
| π1 Gruis | 21 | ? | 535 | S5,7 | ||
| Aldebaran (α Tauri) | 20.58–21.1 | LD | 65.3 | K5+III | ||
| GY Aquilae | 20.46 | ? | 1108 | M8 | ||
| R Lyrae | 18.016 | LD | 310 | M4.5III | ||
| Scheat (β Pegasi) | 16.75 | Ross | 196 | M2.5II-III | ||
(ρ Persei) | 16.555 | LD | 308 | M4+IIIa | ||
| SW Virginis | 16.11–16.8 | UD | 527 | M7III: | ||
| R Aquarii | 15.6116.59 | LD | 711 | M6.5–M8.5e | ||
| g Herculis | 15.219.09 | LD | 385 | M6-III | ||
| RS Cancri | 15.117.2 | LD | 490 | M6S | ||
| Tejat (μ Geminorum) | 15.118 | LD | 230 | M3IIIab | ||
| R Leonis Minoris | 14.4 | LD | 942 | M6.5-9e | ||
| S Cephei | 14.29 | LD | 1591 | C7,3e | ||
| T Cassiopeiae | 14.22 | LD | 893 | M7-9e | ||
| μ Cephei (Herschel's Garnet Star) | 14.11 ± 0.6[13] | 3060[14] | M2Ia | |||
| Mirach (β Andromedae) | 13.749 | LD | 199 | M0+IIIa | ||
| Menkar (α Ceti) | 13.238 | LD | 249 | M1.5IIIa | Other measurements include 12.2 mas. | |
| V Cygni | 13.114.84 | LD | 1747 | C7,4eJ |