List of largest stars
Appearance
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Below is a list of the largest known stars by radius. The unit of measurement used is the radius of the Sun (approximately 695,500 kilometers, or 432,450 miles).
The exact order of this list is not complete yet, nor is it perfectly defined:
- There are sometimes high uncertainties in derived values and sizes;
- The distances to most of these stars are uncertain to differing degrees and this uncertainty affects the size measurements;
- Several large stars have extended atmospheres, are embedded in mostly opaque dust shells or disks, and pulsate, such that determining their radii is not well defined;
- There are theoretical reasons for expecting that no stars in our galaxy are larger than approximately 1,500 times the sun, based on evolutionary models and the Hayashi instability zone. The exact limit depends on the metallicity of the star, so for example supergiants in the Magellanic Clouds have slightly different limiting temperature and luminosity. Stars exceeding the limit have been seen to undergo large eruptions and to change their spectral type over just a few months;
- A survey of the Magellanic Clouds[1] has catalogued most of the red supergiants and 44 of them are larger than the 700 solar radii cutoff point of this table, with the largest at 1,200-1,300.
List
Star name | Solar radii (Sun = 1) |
Notes | ||
---|---|---|---|---|
NML Cygni | 1,650[2] | |||
V838 Monocerotis | 1,570 ± 400 [3] | The very large cool "L supergiant" reported with this radius was a transient object that shrunk about four-fold over a few years. 380 solar radii as of 2009.[4] | ||
WOH G64 | 1,540[5] | This would be the largest star in the LMC, but is unusual in position and motion and might still be a foreground halo giant. | ||
VX Sagittarii | 1,520[6] | VX Sgr is a pulsating variable with a large visual range and varies significantly in size. | ||
KW Sagittarii | 1,460[7] | |||
KY Cygni | 1,420–2,850 [7] | The upper estimate is due to an unusual K band measurement and thought to be an artifact of a reddening correction error. The lower estimate is consistent with other stars in the same survey and with theoretical models. | ||
Westerlund 1-26 | 1,951–2,544 [8][9][10] | Very uncertain parameters for an unusual star with strong radio emission. The spectrum is variable but apparently the luminosity is not. | ||
VY Canis Majoris | 1,420 | Once thought to be a star so large that it contradicted stellar evolutionary theory, improved measurements have brought it down to size.[11][12] | ||
RW Cephei | 1,260–1,610 [citation needed] | RW Cep is variable both in brightness (by at least a factor of 3) and spectral type (observed from G8 to M), thus probably also in diameter. Because the spectral type and temperature at maximum luminosity are not known, the quoted sizes are just estimates. | ||
PZ Cassiopeiae | 1,190-1,940[7] | The upper estimate is due to an unusual K band measurement and thought to be an artifact of a reddening correction error. The lower estimate is consistent with other stars in the same survey and with theoretical models. | ||
VV Cephei A | 1,050–1,900 | VV Cep A is a highly distorted star in a close binary system, losing mass to the secondary for at least part of its orbit. | ||
Mu Cephei (Herschel's "Garnet Star") | 650[13]-1,420[7] | |||
BI Cygni | 916[6]-1,240[7] | |||
V354 Cephei | 690[6]-1,520[7] | |||
S Persei | 780-1,230[7] | In the Perseus Double Cluster | ||
BC Cygni | 1,140[7] | |||
RT Carinae | 1,090[7] | |||
V396 Centauri | 1,070[7] | |||
CK Carinae | 1,060[7] | |||
V1749 Cygni | 620-1,040[7] | |||
RS Persei | 1,000[7] | In the Perseus Double Cluster | ||
NR Vulpeculae | 980[7] | |||
RW Cygni | 980[7] | |||
V602 Carinae | 860[7] | |||
Betelgeuse (Alpha Orionis) | 1,000-3,000[14] | |||
Antares (Alpha Scorpii) A | 949 | |||
TZ Cassiopeiae | 800[7] | |||
IX Carinae | 790[7] | |||
SU Persei | 780[7] | In the Perseus Double Cluster | ||
TV Geminorum | 770[7] | |||
V355 Cephei | 300[6]-770[7] | |||
V382 Carinae | 700 | |||
The following well-known stars are listed for the purpose of comparison. | ||||
CE Tauri ("Ruby Star")[15] | 608 | |||
S Pegasi | 580[16] | |||
W Hydrae | 562[17] | |||
T Cephei | 540[18] | |||
S Orionis | 530[19] | |||
R Cassiopeiae | 500[20] | |||
R Leporis | 500 | |||
R Andromedae | 485 ± 125 | |||
Chi Cygni | 470[21] | |||
Alpha Herculis (Ras Algethi) | 460 | |||
R Hydrae | 460 | |||
Rho Cassiopeiae | 450 | |||
Mira A (Omicron Ceti) | 400[22] | |||
V509 Cassiopeiae | 400[23]–900[24] | |||
S Doradus | 100–380[25] | |||
U Orionis | 370±96 | |||
R Doradus | 370 | |||
HR Carinae | 350 | |||
R Leonis | 350[26] | |||
V337 Carinae | 350 | |||
The Pistol Star | 340 | |||
S Coronae Borealis | 340 | |||
V381 Cephei | 327 | |||
Pi Puppis | 290 | |||
Psi1 Aurigae | 271 | |||
CW Leonis | 250 | |||
Cygnus OB2-12 | 246 | |||
Omicron1 Canis Majoris | 231 | |||
La Superba (Y Canum Venaticorum) | 215 | |||
Delta Canis Majoris (Wezen) | 215±66[27] | |||
V810 Centauri | 210 | |||
Zeta Aurigae (Haedus) | 200[28] | |||
Delta2 Lyrae | 200 | |||
Lambda Velorum (Al Suhail) | 200 | |||
RS Puppis | 200 | |||
Eta Carinae (Tseen She) | 85–195[29] | Previously thought to be the most massive single star, but in 2005 it was realised to be a binary system | ||
Epsilon Pegasi (Enif) | 185 | |||
L Carinae | 179 | |||
6 Cassiopeiae | 170 | |||
Rho Persei (Gorgonea Tertia) | 164 | |||
Epsilon Carinae (Avior) | 153 | |||
Gamma Cygni (Sadir) | 150 | |||
LBV 1806-20 | 150 | |||
Epsilon Geminorum (Mebsuta) | 150 | |||
Epsilon Aurigae A (Almaaz) | 135 | |||
Mu Boötis (Alkalurops) | 130 | |||
66 Andromedae | 130 | |||
QS Aquilae | 130 | |||
NO Aurigae | 130 | |||
56 Aquilae | 130 | |||
L Puppis | 126 | |||
Iota Scorpii (Apollyon) | 125 | |||
Delta Apodis | 125 | |||
HIP 110307 | 124.1 | |||
32 G. Hydrae | 121.7 | |||
I Carinae | 120 | |||
Xi Puppis (Asmidiske) | 120 | |||
Mu Sagittarii (Polis) | 115 | |||
Omicron Cygni | 115 | |||
Deneb | 114 | |||
V533 Carinae (VV Storm) | 114 | |||
Gamma Crucis (Gacrux) | 113[30] | |||
Zeta Cephei | 110 | |||
Gamma Aquilae (Tarazed) | 110 | |||
34 Boötis | 110 | |||
Beta Arae | 110 | |||
Alpha Trianguli Australis (Atria) | 109 | |||
Peony Nebula Star | 100 | |||
Beta Pegasi (Scheat) | 95 | |||
17 Camelopardalis | 91.3 | |||
Beta Andromedae (Mirach) | 90 | |||
R Scuti | 87.4 | |||
WR 102ea | 86 | |||
Nu Cephei | 83.5 | |||
Gamma Andromedae (Almach) | 83 | |||
Theta Herculis (Rukbalgethi Genubi) | 80 | |||
Var 83 | 80 | |||
Rigel (Beta Orionis) | 78 | |||
Alpha Leporis (Arneb) | 77 | |||
P Cygni | 76 | |||
Beta Doradus | 76 | |||
DL Crucis | 75-80 | |||
Pi Herculis | 72 | |||
13 Boötis | 71 | |||
R Leporis | 70.4 | |||
Beta Cygni A1 (Albireo) | 70 | |||
62 Sagittarii | 70 | |||
Nu Aquilae (Equator Star) | 66 | |||
R Coronae Borealis | 65 | |||
Canopus (Alpha Carinae) | 65 | |||
Delta Virginis (Auva) | 65 | |||
Delta Sagittarii (Kaus Media) | 62 | |||
Alpha Persei (Mirfak) | 60 | |||
Zeta Geminorum (Mekbuda) | 60 | |||
Eta Aquilae (Bezek) | 60 | |||
89 Herculis | 60 | |||
Upsilon Sagittarii | 60 | |||
Alpha Aquarii (Sadalmelik) | 60 | |||
CPD -572874 | 60 | |||
Chi Orionis | 59 | |||
Alpha Persei (Mirfak) | 56 | |||
Iota Aurigae (Al Kab) | 55 | |||
FF Aquilae | 55 | |||
Alpha Apodis | 55 | |||
Tau Serpentis | 54 | |||
Beta Cancri (Tarf) | 53 | |||
Alpha Antliae | 53 | |||
Zeta¹ Scorpii | 52 | |||
Alphard (Alpha Hydrae) | 50.5 | |||
Gamma Draconis (Eltanin) | 50 | |||
Beta Aquarii (Sadalsuud) | 50 | |||
HD 5980 A | 48-160 | |||
Epsilon Boötis (Izar) | 48 | |||
Zeta² Scorpii | 48 | |||
AG Antliae | 47 | |||
V428 Andromedae | 46.3 | |||
HD 13189 | 46 | |||
HD 203857 | 46 | |||
Aldebaran (Alpha Tauri) | 44.2[31] | |||
Polaris (Alpha Ursae Minoris) | 43.9 | |||
Alpha Cassiopeiae (Schedar) | 42 | |||
Alpha Ceti (Menkar) | 42 | |||
Delta Cephei (Alrediph) | 41.6 | |||
Beta Ursae Minoris (Kochab) | 41 | |||
Beta Draconis (Rastaban) | 40 | |||
BD Camelopardalis | 40 | |||
HD 5980 B | 40 | |||
Eta Canis Majoris (Aludra) | 37.8 | |||
87 Leonis | 37 | |||
Gamma Centauri (Muhlifan) | 36.5 | |||
S Normae | 35.6 | |||
R136a1 | 35.4 | Also on record as the most massive and luminous star known. | ||
Sher 25 | 35 | |||
Gamma Leonis (Algieba) | 31.9 | |||
Alpha Camelopardalis | 31.2 | |||
Alpha Ursae Majoris (Dubhe) | 30 | |||
11 Lacertae | 30 | |||
Beta Camelopardalis | 30 | |||
Cygnus OB2-8 | 28 | |||
Eta Leonis (Al Jabhah) | 27 | |||
R Apodis | 26.3 | |||
Epsilon Orionis (Alnilam) | 26 | |||
Eta Piscium (Kullat Nunu) | 26 | |||
Melnick 42 | 26 | |||
Arcturus (Alpha Boötis) | 25.7 | |||
HD 93129A | 25 | |||
11 Ursae Minoris | 24.1 | |||
HD 47536 | 23.5 | |||
Epsilon Leonis (Algenubi) | 23 | |||
42 Draconis | 22 ± 1 | |||
Alpha Reticuli | 21 | |||
Chi Virginis | 20.9 | |||
19 Cephei | 20–30 | |||
HDE226868 | 20-22 | The supergiant companion of Cygnus X-1 | ||
Zeta Orionis (Alnitak) | 20 | |||
Theta Scorpii (Sargas) | 20 | |||
Beta Herculis (Kornephoros) | 20 | |||
Theta Apodis | 20 | |||
Alpha Sagittae (Alsahm) | 20 | |||
HR 2422 Monocerotis (Plaskett's Star) | 19.2 | |||
Kappa Cassiopeiae | 19 | |||
Beta Scorpii (Acrab) | 19 | |||
Beta Lyrae (Sheliak) | 19 | |||
Zeta Puppis (Naos) | 18.6 | |||
R 122 | 18.5 | |||
HD 93250 | 18 | |||
Alpha Microscopii | 17.5 | |||
LH45-425 A | 17.5 | |||
Upsilon Hydrae | 17.1 | |||
Beta Ceti (Deneb Kaitos) | 17 | |||
Epsilon Canis Majoris (Adhara) | 17 | |||
LY Aurigae | 16 | |||
Theta Centauri (Menkent) | 16 | |||
Beta Corvi (Kraz) | 16 | |||
Delta Orionis A (Mintaka) | 15.8 | |||
Nu Ophiuchi (Sinistra) | 15.25 | |||
Alpha Arietis (Hamal) | 15 | |||
Gamma Cassiopeiae (Tsih) | 14 | |||
Beta Ophiuchi (Celbalrai) | 13.2 | |||
37 Aquilae | 13 | |||
HD 240210 | 13 | |||
Alpha Aurigae A (Capella A) | 12.2 | |||
Xi Aquilae | 12 | |||
Gamma Arae | 12 | |||
Gamma Sagittarii (Alnasl) | 11 | |||
LH45-425 B | 10 | |||
VV Cephei B | 10 |
See also
- Constellation
- Lists of stars
- List of most massive stars
- List of most luminous stars
- TrES-4, one of the largest known planets
References
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|doi=10.1051/0004-6361/201219587
instead. - ^ B. F. Lane, A. Retter, R. R. Thompson, J. A. Eisner (April 2005). "Interferometric Observations of V838 Monocerotis". The Astrophysical Journal Letters. 622 (2): L137–L140. arXiv:astro-ph/0502293. Bibcode:2005ApJ...622L.137L. doi:10.1086/429619.
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: CS1 maint: multiple names: authors list (link) - ^ Attention: This template ({{cite doi}}) is deprecated. To cite the publication identified by doi:10.1051/0004-6361/201116858 , please use {{cite journal}} (if it was published in a bona fide academic journal, otherwise {{cite report}} with
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Emily M. Levesque, Philip Massey, Bertrand Plez, and Knut A. G. Olsen (June 2009). "The Physical Properties of the Red Supergiant WOH G64: The Largest Star Known?". Astronomical Journal. 137 (6): 4744. arXiv:0903.2260. Bibcode:2009AJ....137.4744L. doi:10.1088/0004-6256/137/6/4744.
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- ^ a b c d e f g h i j k l m n o p q r s t u Table 4 in Emily M. Levesque, Philip Massey, K. A. G. Olsen, Bertrand Plez, Eric Josselin, Andre Maeder, and Georges Meynet (August 2005). "The Effective Temperature Scale of Galactic Red Supergiants: Cool, but Not As Cool As We Thought". The Astrophysical Journal. 628 (2): 973–985. arXiv:astro-ph/0504337. Bibcode:2005ApJ...628..973L. doi:10.1086/430901.
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: CS1 maint: multiple names: authors list (link) - ^ Attention: This template ({{cite doi}}) is deprecated. To cite the publication identified by doi:10.1051/0004-6361/201116990, please use {{cite journal}} (if it was published in a bona fide academic journal, otherwise {{cite report}} with
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instead. - ^ Fok; Jun-ichi Nakashima; Yung; Chih-Hao Hsia; Shuji Deguchi (2012). "Maser Observations of Westerlund 1 and Comprehensive Considerations on Maser Properties of Red Supergiants Associated with Massive Clusters". arXiv:1209.6427v1 [astro-ph.SR].
- ^ Attention: This template ({{cite doi}}) is deprecated. To cite the publication identified by doi:10.1051/0004-6361/200913820, please use {{cite journal}} (if it was published in a bona fide academic journal, otherwise {{cite report}} with
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instead. - ^ Attention: This template ({{cite doi}}) is deprecated. To cite the publication identified by doi:10.1051/0004-6361/201219126, please use {{cite journal}} (if it was published in a bona fide academic journal, otherwise {{cite report}} with
|doi=10.1051/0004-6361/201219126
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Y. K. Choi; Hirota; Honma; Kobayashi; Bushimata; Imai; Iwadate; Jike; Kameno (2008). "Distance to VY VMa with VERA". Publications of the Astronomical Society of Japan. 60. Publications Astronomical Society of Japan: 1007. arXiv:0808.0641. Bibcode:2008PASJ...60.1007C.
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specified (help) - ^ Tsuji, Takashi (2000). "Water in Emission in the Infrared Space Observatory Spectrum of the Early M Supergiant Star μ Cephei". The Astrophysical Journal Letters. 540 (2): 99–102. arXiv:astro-ph/0008058. Bibcode:2000ApJ...540L..99T. doi:10.1086/312879.
- ^ Graham M. Harper; et al. (2008). "A NEW VLA-HIPPARCOS DISTANCE TO BETELGEUSE AND ITS IMPLICATIONS". The Astronomical Journal. 135 (4): 1430–1440. Bibcode:2008AJ....135.1430H. doi:10.1088/0004-6256/135/4/1430.
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- ^ Nugent, Richard. "The Garnet Star". weblore.com. Retrieved 2009-12-04.
DIAM .. m Cep 1224 ... V509 CAS 910 ... V382 CAR 747
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ignored (help) - ^ Fedele; Wittkowski; Paresce; Scholz; Wood; Ciroi (2004). "The K-band intensity profile of R Leonis probed by VLTI/VINCI". Astronomy and Astrophysics. 431 (3): 1019–1026. arXiv:astro-ph/0411133. Bibcode:2005A&A...431.1019F. doi:10.1051/0004-6361:20042013.
- ^ Davis J, Booth AJ, Ireland MJ, Jacob AP, North JR, Owens SM, Robertson JG, Tango WJ, Tuthill PG, J.; Booth, A. J.; Ireland, M. J.; Jacob, A. P.; North, J. R.; Owens, S. M.; Robertson, J. G.; Tango, W. J.; Tuthill, P. G. (2007). "The Emergent Flux and Effective Temperature of Delta Canis Majoris". Publications of the Astronomical Society of Australia. 24 (3): 151. arXiv:0709.3873. Bibcode:2007PASA...24..151D. doi:10.1071/AS07017.
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: CS1 maint: multiple names: authors list (link) - ^ "Zeta Aurigae". Hposoft.com. Retrieved 2012-10-14.
- ^ "The HST Treasury Program on Eta Carinae". Etacar.umn.edu. 2003-09-01. Retrieved 2012-10-14.
- ^ Gamma Crucis by Jim Kaler
- ^ Richichi, A.; Roccatagliata, V. (2005). "Aldebaran's angular diameter: how well do we know it?". Astronomy and Astrophysics. 433: 305–312. arXiv:astro-ph/0502181. Bibcode:2005A&A...433..305R. doi:10.1051/0004-6361:20041765.