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VY CMa 1420 Rsol estimate uses an accurate parallax and an accurate angular diameter - 1420 Rsol estimate IS accurate. Also added a few newer star parameters
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! colspan="4" style="background:#efefef" class="sortbottom" | The above radii are larger than what [[stellar evolution]] theory predicts, and are thus potentially unreliable


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|This 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 simply do not form.<ref name="levesque-2"/><br/><small>Reported for reference</small>
|This 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 simply do not form.<ref name="levesque-2"/><br/><small>Reported for reference</small>
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|{{val|780|156|fmt=commas}}(–{{val|1230|246|fmt=commas}})<ref name="levesque-2"/>, 1,364<ref>{{Cite journal|last=Norris|first=Ryan|date=2019-08-13|title=Seeing Stars Like Never Before: A Long-term Interferometric Imaging Survey of Red Supergiants|url=https://scholarworks.gsu.edu/phy_astr_diss/118|journal=Physics and Astronomy Dissertations}}</ref>
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|1,356<ref>{{Cite journal|last=Tabernero|first=H. M.|last2=Dorda|first2=R.|last3=Negueruela|first3=I.|last4=Marfil|first4=E.|date=2021-02|title=On the nature of VX Sagitarii: Is it a TZO, a RSG or a high-mass AGB star?|url=http://arxiv.org/abs/2011.09184|journal=Astronomy & Astrophysics|volume=646|pages=A98|doi=10.1051/0004-6361/202039236|issn=0004-6361}}</ref>
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|V766 Centauri Aa is a rare variable [[yellow supergiant]].
|V766 Centauri Aa is a rare variable [[yellow supergiant]].
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|[[RT Carinae]]
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|1,074<ref>{{Cite journal|last=Massalkhi|first=S.|last2=Agúndez|first2=M.|last3=Cernicharo|first3=J.|date=2019-08|title=Study of CS, SiO, and SiS abundances in carbon star envelopes: Assessing their role as gas-phase precursors of dust|url=http://arxiv.org/abs/1906.09461|journal=Astronomy & Astrophysics|volume=628|pages=A62|doi=10.1051/0004-6361/201935069|issn=0004-6361}}</ref>
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|[[Westerlund 1-20|Westerlund 1 W20]] ''(Westerlund 1 BKS D)''
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! colspan="4" | The following well-known stars are listed for the purpose of comparison.
! colspan="4" | The following well-known stars are listed for the purpose of comparison.
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Revision as of 19:21, 19 February 2022

Not to be confused with List of most massive stars.

Relative sizes of the planets in the Solar System and several well-known 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 695,700 km; 432,300 mi).[1]

The angular diameters of stars can be measured directly using stellar interferometry. Other methods can use lunar occultations or from eclipsing binaries, which can be used to test indirect methods of finding stellar radii. Only a few useful supergiant stars can be occulted by the Moon, including Antares A (Alpha Scorpii A). Examples of eclipsing binaries are Epsilon Aurigae (Almaaz), VV Cephei, and V766 Centauri (HR 5171). Angular diameter measurements can be inconsistent because the boundary of the very tenuous atmosphere (opacity) differs depending on the wavelength of light in which the star is observed.

Uncertainties remain with the membership and order of the lists, especially when deriving various parameters used in calculations, such as stellar luminosity and effective temperature. Often stellar radii can only be expressed as an average or be within a large range of values. Values for stellar radii vary significantly in different sources and for different observation methods.

All the sizes stated in these lists have inaccuracies and may be disputed. The lists are still a work in progress and parameters are prone to change.

Caveats

Various issues exist in determining accurate radii of the largest stars, which in many cases do display significant errors. The following lists are generally based on various considerations or assumptions; these include:

  • Stellar radii or diameters are usually derived only approximately using 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 supergiant stars have extended atmospheres, and many are within opaque dust shells, making their true effective temperatures and surfaces highly uncertain.[citation needed]
  • 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.
  • Most 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).[2][3]

Lists

The following lists show the largest known stars based on the host galaxy.

Milky Way

List of the largest known stars in the Milky Way[a]
Star name Solar radii
(Sun = 1) 		Method[b] Notes
Orbit of Saturn 2,047–2,049.9[4][c] Reported for reference
V1489 Cygni (NML Cygni) 1,639 – 2,770[5] L/Teff
The above radii are larger than what stellar evolution theory predicts, and are thus potentially unreliable
Theoretical limit of star size (Milky Way) ~1,500[6] This 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 simply do not form.[6]
Reported for reference
KY Cygni 1,420±284–(2,850±570)[6] L/Teff
VY Canis Majoris 1,420±120[7] AD
AH Scorpii 1,411±124[8] AD
GCIRS 7 1,170±60[9]–1,368[10] AD
S Persei 780±156(–1,230±246)[6], 1,364[11] L/Teff
VX Sagittarii 1,356[12]

853[13]-1,335±215[14]

L/Teff
Westerlund 1 W237 (Westerlund 1 BKS B) 1,241±70[15] L/Teff
BC Cygni 1,230.27[16]–1,140±228[6] 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.[17]
IRC -10414 ~1,200[18] L/Teff
PZ Cassiopeiae 1,190±238(–1,940±388)[6] L/Teff
Westerlund 1 W26 (Westerlund 1 BKS AS) 1,165±58–1,221±120[15] L/Teff
Orbit of Jupiter 1,114.5–1,115.8[4][c] Reported for reference
V766 Centauri Aa 1,110±50[19] ? V766 Centauri Aa is a rare variable yellow supergiant.
RT Carinae 1,090±218[6] L/Teff
LL Pegasi 1,074[20] L/Teff
V396 Centauri 1,070±214[6] – 1,145.31[21] L/Teff & ?
V602 Carinae 1,050±165[22] AD
CK Carinae 1,013.42 – 1,060±212[6] L/Teff
KW Sagittarii 1,009±142[8] AD
AZ Cygni 911+57
−50[23] 		AD
NSV 25875 891[13] L/Teff
V437 Scuti 874[13] L/Teff
V669 Cassiopeiae 859[13] L/Teff
Westerlund 1 W20 (Westerlund 1 BKS D) 858±48[15] L/Teff
BI Cygni 851.14[16]–1,240±248[6] L/Teff
μ Cephei (Herschel's Garnet Star) 830[13]-972±228[24] AD
V1185 Scorpii 830[13] L/Teff
CW Leonis 826[13] L/Teff
LP Andromedae 815[13] L/Teff
RT Ophiuchi 801±217[25] AD
BO Carinae 790±158[6] L/Teff
SU Persei 780±156[6] – 971.405[21] L/Teff
RS Persei 770±30[26] AD
V355 Cephei 770±154[6] L/Teff
GU Cephei A 766.486[21] ?
Betelgeuse (α Orionis) 764+116
−62[27] 		? Tenth brightest star in the night sky.[28]
HD 303250 750±150[6] L/Teff
UU Pegasi 742±193[25] AD
Westerlund 1 W75 (Westerlund 1 BKS E) 722±36[15] L/Teff
V Camelopardalis 716±185[25] AD
V923 Centauri 715.539[21] ?
V528 Carinae 700±140[6] L/Teff The following well-known stars are listed for the purpose of comparison.
V354 Cephei L/Teff
Antares A (α Scorpii) 680[29] AD Fourteenth brightest star in the night sky.[28]
RW Cygni 676.08[16] – 980±196[6] – 1,502.16[21] ?
6 Geminorum (BU Geminorum) 670±134[6] L/Teff
TZ Cassiopeiae 645.65,[16] 766.813[21] – 800±160[6] L/Teff
R Hydrae 631[13] L/Teff
NO Aurigae 630±126[6] – 1,481.85[21] L/Teff
DU Crucis 629.63[21] ?
IX Carinae 620.718[21]920±184[6] L/Teff
TV Geminorum ~620–710[30] L/Teff
R Sculptoris 617[13] L/Teff
V Hydrae 609[13] L/Teff
V419 Cephei 590±118[6] L/Teff
119 Tauri (CE Tauri) 587±85–593±86[31] AD
R Leonis Minoris 569±146[25] AD
TX Camelopardalis 560[13] L/Teff
S Orionis 545±142[25] AD
Mira A (ο Ceti) 541[13] L/Teff
VV Cephei A 515.632[21] – 1,050[32] ? & AD
T Persei 510±20[26] – 622.081[21] AD
V1427 Aquilae 507[13] L/Teff
HR Carinae B 500±150[33] AD
QY Puppis 485.319[21] ?
V838 Monocerotis 464[34]–730[35] ? & AD
S Pegasi 459±135[25] AD
S Coronae Borealis 457±116[25] AD
IK Tauri (NML Tauri) 451[13] L/Teff
π1 Gruis 447[13] L/Teff
R Aquarii 438±114[25] AD
U Herculis 431±114[25] AD
NR Vulpeculae 426.58,[16] 668.395[21]–980±196[6] L/Teff
Unurgunite (σ Canis Majoris) 420±84[6] L/Teff
V810 Centauri 420[36] L/Teff
W Aquilae 419[13] L/Teff
R Cassiopeiae 410[13] - 593±181[25] L/Teff & AD
R Aurigae 407±105[25] AD
R Leporis 400±90[37] ?
U Hydrae 395[13] L/Teff
S Scuti 386[13] L/Teff
MZ Puppis 376.973[21] ?
Westerlund 1 W243 (Westerlund 1 BKS G) 376.9[38] ?
U Orionis 370±96[25] AD
R Aquilae 354±99[25] AD
V4650 Sagittarii 350[39] ?
R Serpentis 328±86[25] AD
U Antliae 325[13] L/Teff
Orbit of Mars 322–323.1[4][c] Reported for reference
5 Lacertae (V412 Lacertae) 319.2+26.6
−32.0[40] 		AD
T Ceti 312[13] L/Teff
Y Canum Venaticorum (La Superba) 307[13] L/Teff
Pistol Star (V4647 Sagittarii) 306[39] ?
R Leonis 299[13] - 409±105[25] AD & L/Teff
R Doradus (P Doradus) 298±21[41] AD
S Ursae Minoris 296±82[25] AD
Rasalgethi A (α Herculis) 284±60 (264–303)[42] L/Teff
ο1 Canis Majoris 280±56[6] L/Teff
R Canum Venaticorum 279±75[25] AD
R Aquilae 259±67[25] AD
S Doradus 240±140[43] ?
V424 Lacertae 239±80[44]–260±52[6] AD & L/Teff
SW Cephei 234.42[16] L/Teff
W Hydrae 229[13] L/Teff
NGC 6910 RLP 10 (Cygnus OB2-12) 229[45] L/Teff
HR Carinae A 220±60[33] AD
Wezen (δ Canis Majoris) 215±66[46] AD Thirty-sixth brightest star in the night sky.[28]
Orbit of Earth (~1 AU) 214[4][c] Reported for reference
Enif (ε Pegasi) 210.37 – 210.69[47] ?
Suhail (λ Velorum) 210[48] ?
Deneb (α Cygni) 203±17[49] ? Eighteenth brightest star in the night sky.[28]
Orbit of Venus 158.6[4][c] Reported for reference
Orbit of Mercury 82.9–84.6[4][c] Reported for reference
Vega (α Lyrae) 2.726±0.006 × 2.418±0.012[50] Fifth brightest star in the night sky.[28]
Reported for reference
Sun 1 The largest object in the Solar System.
Reported for reference

Magellanic Clouds

List of the largest known stars in the Magellanic Clouds
Star name Solar radii
(Sun = 1) 		Galaxy Method[d] Notes
WOH G64 1,540[51] Large Magellanic Cloud L/Teff Surrounded by a large dust cloud.

Other galaxies (within the Local Group)

List of the largest known stars in other galaxies (within the Local Group)
Star name Solar radii
(Sun = 1) 		Galaxy Method[e] Notes
Sextans A 10 995±130[52] Sextans A L/Teff
Sextans A 5 870±145[52] Sextans A L/Teff
Sextans A 7 710±100[52] Sextans A L/Teff
IC 10 3 685±90[52] IC 10 L/Teff
WLM 14 610±80[52] WLM L/Teff
Sextans B 1 565±70[52] Sextans B L/Teff
IC 1613 2 560±70[52] IC 1613 L/Teff
WLM 12 430±70[52] WLM L/Teff
IC 10 5 420±50[52] IC 10 L/Teff
Sextans B 2 405±90[52] Sextans B L/Teff
WLM 13 380±50[52] WLM L/Teff
Sextans A 6 350±40[52] Sextans A L/Teff
Pegasus 1 340±50[52] Pegasus Dwarf L/Teff
Sextans A 4 335±40[52] Sextans A L/Teff
WLM 11 310±50[52] WLM L/Teff
IC 1613 1 300±40[52] IC 1613 L/Teff
IC 10 2 280±30[52] IC 10 L/Teff
Pegasus 2 260±40[52] Pegasus Dwarf L/Teff
Sextans A 8 260±60[52] Sextans A L/Teff
Sextans A 9 230±50[52] Sextans A L/Teff
IC 10 4 200±25[52] IC 10 L/Teff
IC 10 1 165±60[52] IC 10 L/Teff
IC 10 6 160±25[52] IC 10 L/Teff
Phoenix 3 90±15[52] Phoenix Dwarf L/Teff

Outside the Local Group

List of the largest known stars in galaxies outside the Local Group
Star name Solar radii
(Sun = 1) 		Galaxy Group Method[f] Notes
NGC 2363-V1 194–356[53] NGC 2363 M81 Group ?

Notes

  1. ^ Currently only contains radii that are stated in the cited papers
  2. ^ Methods for calculating the radius:
  3. ^ a b c d e f At the J2000 epoch
  4. ^ Methods for calculating the radius:
  5. ^ Methods for calculating the radius:
  6. ^ Methods for calculating the radius:

References

  1. ^ 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. Bibcode:2015arXiv151007674M. {{cite journal}}: Cite journal requires |journal= (help)
  2. ^ 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: 1102–1117. arXiv:astro-ph/0603596. Bibcode:2006ApJ...645.1102L. doi:10.1086/504417. ISSN 0004-637X.
  3. ^ Ren, Yi; Jiang, Bi-Wei (July 2020). "On the Granulation and Irregular Variation of Red Supergiants". The Astrophysical Journal. 898: 24. arXiv:2006.06605. Bibcode:2020ApJ...898...24R. doi:10.3847/1538-4357/ab9c17. ISSN 0004-637X.{{cite journal}}: CS1 maint: unflagged free DOI (link)
  4. ^ a b c d e f "HORIZONS Web-Interface". ssd.jpl.nasa.gov. Retrieved 2021-09-25.
  5. ^ Zhang, B.; Reid, M. J.; Menten, K. M.; Zheng, X. W.; Brunthaler, A. (August 2012). "The Distance and Size of the Red Hypergiant NML Cyg from VLBA and VLA Astrometry". Astronomy & Astrophysics. 544: A42. doi:10.1051/0004-6361/201219587. ISSN 0004-6361.
  6. ^ a b c d e f g h i j k l m n o p q r s t u v w x y Levesque, Emily M.; Massey, Philip; Olsen, K. A. G.; Plez, Bertrand; Josselin, Eric; Maeder, Andre; Meynet, Georges (August 2005). "The Effective Temperature Scale of Galactic Red Supergiants: Cool, but Not As Cool As We Thought". The Astrophysical Journal. 628: 973–985. arXiv:astro-ph/0504337. Bibcode:2005ApJ...628..973L. doi:10.1086/430901. ISSN 0004-637X.
  7. ^ Wittkowski, M.; Hauschildt, P.H.; Arroyo-Torres, B.; Marcaide, J.M. (5 April 2012). "Fundamental properties and atmospheric structure of the red supergiant VY CMa based on VLTI/AMBER spectro-interferometry". Astronomy & Astrophysics. 540: L12. arXiv:1203.5194. Bibcode:2012A&A...540L..12W. doi:10.1051/0004-6361/201219126. S2CID 54044968.
  8. ^ a b Arroyo-Torres, B.; Wittkowski, M.; Marcaide, J. M.; Hauschildt, P. H. (June 2013). "The atmospheric structure and fundamental parameters of the red supergiants AH Scorpii, UY Scuti, and KW Sagittarii". Astronomy and Astrophysics. 554: A76. arXiv:1305.6179. Bibcode:2013A&A...554A..76A. doi:10.1051/0004-6361/201220920. ISSN 0004-6361.
  9. ^ Tsuboi, Masato; Kitamura, Yoshimi; Tsutsumi, Takahiro; Miyawaki, Ryosuke; Miyoshi, Makoto; Miyazaki, Atsushi (April 2020). "Sub-millimeter detection of a Galactic center cool star IRS 7 by ALMA". Publications of the Astronomical Society of Japan. 72: 36. arXiv:2002.01620. Bibcode:2020PASJ...72...36T. doi:10.1093/pasj/psaa013. ISSN 0004-6264.
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  11. ^ Norris, Ryan (2019-08-13). "Seeing Stars Like Never Before: A Long-term Interferometric Imaging Survey of Red Supergiants". Physics and Astronomy Dissertations.
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See also

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