View source for Astronomy:List of largest stars

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[[File:Star-sizes.jpg|500px|thumb|right|Relative sizes of the [[Astronomy:Planet|planet]]s in the Solar System and several well-known [[Astronomy:Star|star]]s:
{{ordered list
| [[Astronomy:Mercury (planet)|Mercury]] < [[Astronomy:Mars|Mars]] < [[Astronomy:Venus|Venus]] < [[Astronomy:Earth|Earth]]
| [[Astronomy:Earth|Earth]] < [[Astronomy:Neptune|Neptune]] < [[Astronomy:Uranus|Uranus]] < [[Astronomy:Saturn|Saturn]] < [[Astronomy:Jupiter|Jupiter]]
| [[Astronomy:Jupiter|Jupiter]] < [[Astronomy:Wolf 359|Wolf 359]] < [[Astronomy:Sun|Sun]] < Sirius A
| Sirius A < [[Astronomy:Pollux (star)|Pollux]] < [[Astronomy:Arcturus|Arcturus]] < [[Astronomy:Aldebaran|Aldebaran]]
| [[Astronomy:Aldebaran|Aldebaran]] < Rigel A < Antares A < [[Astronomy:Betelgeuse|Betelgeuse]]| [[Astronomy:Betelgeuse|Betelgeuse]] < [[Astronomy:Mu Cephei|Mu Cephei]] < [[Astronomy:VV Cephei A|VV Cephei A]] < [[Astronomy:VY Canis Majoris|VY Canis Majoris]]
}}
]]
Below is a '''list of the largest stars''' currently known, ordered by [[Radius|radius]]. The unit of measurement used is the [[Astronomy:Solar radius|radius of the Sun]] (approximately {{convert|1|solar radius|km mi|sigfig=4|abbr=on|disp=out|lk=on}}).

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

Uncertainties remain with the membership and order of the list, especially when deriving various parameters used in calculations, such as stellar [[Astronomy:Luminosity|luminosity]] and [[Astronomy:Effective temperature|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 this list have various inaccuracies and may be disputed. This list is still a work in progress and various parameters are extremely disputed.
==Caveats==

[[File:Star Sizes Comparison update 2021.png|thumb|right|420px|Comparison of the sizes of several stars. From left to right are [[Astronomy:Cygnus OB2-12|Cygnus OB2#12]] (blue hypergiant), V382 Carinae (yellow hypergiant), V915 Scorpii (orange hypergiant) and the extreme red supergiants UY Scuti and Stephenson 2-18. The orbits of Saturn and Neptune are also shown for comparison.]]

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 [[Physics:Stefan–Boltzmann law|Stefan–Boltzmann law]] for the deduced stellar [[Astronomy:Luminosity|luminosity]] and [[Astronomy:Effective temperature|effective surface temperature]].
* [[Astronomy:Stellar distance|Stellar distance]]s, 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|date=December 2020}}
* Many extended supergiant atmospheres also significantly change in size over time, regularly or irregularly pulsating over several months or years as [[Astronomy:Variable star|variable star]]s. This makes adopted [[Astronomy:Luminosity|luminosities]] poorly known and may significantly change the quoted radii.
* Other direct methods for determining stellar radii rely on lunar [[Astronomy:Occultation|occultation]]s or from eclipses in binary systems. This is only possible for a very small number of stars.
* In this list are some examples of extremely distant extragalactic stars, which may have slightly different properties and natures than the currently largest-known stars in the [[Astronomy:Milky Way|Milky Way]]. For example, some red [[Astronomy:Supergiant|supergiant]]s in the [[Astronomy:Magellanic Clouds|Magellanic Clouds]] are suspected to have slightly different limiting [[Astronomy:Effective temperature|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).<ref name="mc" /><ref name="ren" />

==List==
 <!-- Do not remove; this list will be incomplete until we map the known universe. -->
{| class="wikitable sortable"
|+List of the largest stars
|-
! style="background:#efefef; white-space:nobr;" width=217px| Star name
! style="background:#ffdead;" width=101px| [[Astronomy:Solar radius|Solar radii]]<br />([[Astronomy:Sun|Sun]] = 1)
! Method{{efn|Methods for calculating the radius:
* AD: radius determined from angular diameter and distance
* L/T<sub>eff</sub>: radius calculated from bolometric luminosity and [[Astronomy:Effective temperature|effective temperature]]
* DSKE: radius calculated using the disk emission
* EB: radius determined from observations of the eclipsing binary|name=|group=}}
! Notes<!--
*** List of stars***
See template documentation (Template:List of largest stars row) for more information about formatting/input
The table break |- does not need to be placed between template calls, but needs to be placed before manually-inserted lines
Every number/pair of numbers must have a reference!
-->
|-
|-
|LGGS J004539.99+415404.1
|1,980<ref name="massey2016" />–2,377<ref name="gordon" />
|L/T<sub>eff</sub>
|Located in the [[Astronomy:Andromeda Galaxy|Andromeda Galaxy]]
|-
|- style="background:Gold;" class="sortbottom"
| Orbit of Saturn || 1,940–2,169 || || <small>Reported for reference</small>
|-
|MSX LMC 597 ''(W60 A27)''
|1,882–1,953<ref name=jones />
|L/T<sub>eff</sub>
|Located in the [[Astronomy:Large Magellanic Cloud|Large Magellanic Cloud]]
|-
|LGGS J004520.67+414717.3
|1,870<ref name="massey2016" />–2,510<ref name="gordon" />
|L/T<sub>eff</sub>
|Located in the [[Astronomy:Andromeda Galaxy|Andromeda Galaxy]]
|-
|[[Astronomy:UY Scuti|UY Scuti]] || 1,708 ± 192<ref name="ArroyoTorres2013" /> || AD || This value was based on an angular diameter and distance of 2.9 kpc. Gaia Data Release 2 suggests a distance of 1.55 kpc and a consequently smaller radius of {{solar radius|755}}.<ref name="messineo2019" /> However, the Gaia parallax is considered unreliable (until further observations) due to a very high level of astrometric noise.<ref name="gaia" />
|-
|LGGS J003919.11+404319.2
|1,685<ref name="massey2021" />
|L/T<sub>eff</sub>
|Located in the [[Astronomy:Andromeda Galaxy|Andromeda Galaxy]]
|-
|WOH S71 ''(LMC 23095)''
|1,662<ref name="steven" />–1,896<ref name="ren" />
|L/T<sub>eff</sub>
|Located in the [[Astronomy:Large Magellanic Cloud|Large Magellanic Cloud]]
|-
|HV 2242 ''(WOH S69)''
|1,645<ref name="ren" />
|L/T<sub>eff</sub>
|Located in the [[Astronomy:Large Magellanic Cloud|Large Magellanic Cloud]]
|-
|-
|LGGS J013339.28+303118.8||1,565<ref name=drout2012 />–1,863<ref name="gordon" />|| L/T<sub>eff</sub> || Located in the [[Astronomy:Triangulum Galaxy|Triangulum Galaxy]]
|-
|[[Astronomy:WOH G64|WOH G64]]
|1,540 ± 77<ref name="University" /><ref name=levesque/>
|L/T<sub>eff</sub>
|Located in the [[Astronomy:Large Magellanic Cloud|Large Magellanic Cloud]]
|-
|LGGS J013312.26+310053.3||1,537<ref name=drout2012 />–1,765<ref name="gordon" />|| L/T<sub>eff</sub> || Located in the [[Astronomy:Triangulum Galaxy|Triangulum Galaxy]]
|-
|MSX LMC 1204 ''(WOH S72)''
|1,537–1,709<ref name=jones />
|L/T<sub>eff</sub>
|Located in the [[Astronomy:Large Magellanic Cloud|Large Magellanic Cloud]]
|-
|-


|-
|W61 8-88 ''(WOH S465)''
|1,491<ref name="ren" />
|L/T<sub>eff</sub>
|Located in the [[Astronomy:Large Magellanic Cloud|Large Magellanic Cloud]]
|-


|-
|[[Astronomy:HV 888|HV 888]] ''(WOH S140)''
|1,477<ref name="kamath" />–1,974<ref name="groenewegen" />
|L/T<sub>eff</sub>
|Located in the [[Astronomy:Large Magellanic Cloud|Large Magellanic Cloud]]. Another recent estimate gives {{solar radius|1,765}}.<ref name="ren" />
|-
|UCAC4 116-007944 ''(MSX LMC 810)''
|1,468<ref name="ren" />
|L/T<sub>eff</sub>
|Located in the [[Astronomy:Large Magellanic Cloud|Large Magellanic Cloud]]
|-
|W60 A78 ''(WOH S459)''
|1,445<ref name="ren" />
|L/T<sub>eff</sub>
|Located in the [[Astronomy:Large Magellanic Cloud|Large Magellanic Cloud]]
|-
|HV 12998 ''(WOH S369)''
|1,443<ref name="ren" />
|L/T<sub>eff</sub>
|Located in the [[Astronomy:Large Magellanic Cloud|Large Magellanic Cloud]]
|-
|W60 A72 ''(WOH S453)''
|1,441<ref name="ren" />
|L/T<sub>eff</sub>
|Located in the [[Astronomy:Large Magellanic Cloud|Large Magellanic Cloud]]
|-



|-
|[[Astronomy:VY Canis Majoris|VY Canis Majoris]]||1,420 ± 120<ref name="gordon2019" /><ref name="wittkowski" />|| AD || Used to be described as the largest known star based on a radius of {{solar radius|1,800–2,100}}.<ref name="humphreys" /> Older estimates gave the radius of VY CMa as above {{solar radius|3,000}},<ref name="monnier" /> or as little as {{solar radius|600}}.<ref name="massey2006" /> Matsuura et al. 2013 estimates {{solar radius|2,069}} based on a luminosity of {{solar luminosity|237,000}} and an assumed effective temperature of 2,800 K.<ref name=matsuura2014 /><ref name=neufeld />
|-
|WOH S286
|1,417<ref name="ren" />
|L/T<sub>eff</sub>
|Located in the [[Astronomy:Large Magellanic Cloud|Large Magellanic Cloud]]
|-
|[[Astronomy:AH Scorpii|AH Scorpii]]
|1,411 ± 124<ref name="ArroyoTorres2013" />
|AD
|AH Sco is a variable by nearly 3 magnitudes in the visual range, and an estimated 20% in luminosity. The variation in diameter is not clear because the temperature also varies.
|-
|LGGS J004428.48+415130.9
|1,410<ref name="massey2016" />–1,504<ref name="gordon" />
|L/T<sub>eff</sub>
|Located in the [[Astronomy:Andromeda Galaxy|Andromeda Galaxy]]
|-
|MG73 46 ''(MSX LMC 891)''
|1,385<ref name="groenewegen" />–1,838<ref name="ren" />
|L/T<sub>eff</sub>
|Located in the [[Astronomy:Large Magellanic Cloud|Large Magellanic Cloud]]
|-
|[[Astronomy:WOH S281|WOH S281]] ''(IRAS 05261-6614)''
|1,376<ref name="Groenewegen" />–1,459<ref name="ren" />
|L/T<sub>eff</sub>
|Located in the [[Astronomy:Large Magellanic Cloud|Large Magellanic Cloud]]
|-
|[[Astronomy:IRAS 05280-6910|IRAS 05280-6910]]
|1,367<ref name=steven/>–1,738<ref name="mikako" />
|L/T<sub>eff</sub>
|Located in the [[Astronomy:Large Magellanic Cloud|Large Magellanic Cloud]]
|-
|[[Astronomy:S Persei|S Persei]]
|1,364 ± 6<ref name="norris" />
|AD
|A [[Astronomy:Red supergiant|red supergiant]] located in the Perseus [[Astronomy:Double Cluster|Double Cluster]]. Levesque ''et al.'' 2005 calculated radii of {{solar radius|780}} and {{solar radius|1,230}} based on [[Physics:K band (infrared)|K-band]] measurements.<ref name="levesqueetal2005" /> Older estimates gave up to {{solar radius|2,853}} based on higher luminosities.<ref name="dejager" />
|-



|-
|[[Astronomy:PHL 293B|PHL 293B]]
|1,348–1,463<ref name=allan />
|L/T<sub>eff</sub>
|A luminous blue variable star located in the low metallicity galaxy [[Astronomy:PHL 293B|PHL 293B]]. It is thought to have disappeared.
|-


|-
|LGGS J013414.27+303417.7||1,342<ref name=drout2012 />–1,953<ref name="gordon" />|| L/T<sub>eff</sub> || Located in the [[Astronomy:Triangulum Galaxy|Triangulum Galaxy]]
|-


|-
|HV 5993 ''(WOH S464)''
|1,319<ref name="groenewegen" />–1,531<ref name="ren" />
|L/T<sub>eff</sub>
|Located in the [[Astronomy:Large Magellanic Cloud|Large Magellanic Cloud]]
|-
|-
|SW Cephei
|1,308<ref name="cruzalebes" />
|AD
|
|-
|Stephenson 2 DFK 2
|1,301<ref name=humphreys2020></ref>
|L/T<sub>eff</sub>
|Located in the massive open cluster Stephenson 2.
|-
|Stephenson 2 DFK 49
|1,300<ref name=humphreys2020>{{cite journal |arxiv=2008.01108 |last1=Humphreys |first1=Roberta M. |last2=Helmel |first2=Greta |last3=Jones |first3=Terry J. |last4=Gordon |first4=Michael S. |title=Exploring the Mass Loss Histories of the Red Supergiants |journal=The Astronomical Journal |year=2020 |volume=160 |issue=3 |page=145 |doi=10.3847/1538-3881/abab15 |bibcode=2020AJ....160..145H |s2cid=220961677 }}</ref>
| L/T<sub>eff</sub>
|Located in the massive open cluster Stephenson 2.
|-



|-
|LGGS J004312.43+413747.1
|1,270<ref name="massey2016" />–1,630<ref name="gordon" />
|L/T<sub>eff</sub>
|Located in the [[Astronomy:Andromeda Galaxy|Andromeda Galaxy]]
|-





|-
|LGGS J004514.91+413735.0
|1,250<ref name="massey2016" />–1,575<ref name="gordon" />
|L/T<sub>eff</sub>
|Located in the [[Astronomy:Andromeda Galaxy|Andromeda Galaxy]]
|-


|-
|LGGS J004428.12+415502.9
|1,240<ref name="massey2016" />–1,259<ref name="gordon" />
|L/T<sub>eff</sub>
|Located in the [[Astronomy:Andromeda Galaxy|Andromeda Galaxy]]
|-




|-
|IRAS 05346-6949
|1,211<ref name="University" />–2,064<ref name=jones />
|L/T<sub>eff</sub>
|Located in the [[Astronomy:Large Magellanic Cloud|Large Magellanic Cloud]]
|-


|-
|LGGS J004125.23+411208.9
|1,200<ref name="massey2016" />–1,602<ref name="gordon" />
|L/T<sub>eff</sub>
|Located in the [[Astronomy:Andromeda Galaxy|Andromeda Galaxy]]
|-




|-
|HD 90587
|1,191<ref name="cruzalebes" />
|AD
|
|-
|[[Astronomy:NML Cygni|NML Cygni]]
|1,183<ref name="debeck" />
|L/T<sub>eff</sub>
|
|-



|-
|LGGS J004524.97+420727.2
|1,170<ref name="massey2016" />–1,476<ref name="gordon" />
|L/T<sub>eff</sub>
|Located in the [[Astronomy:Andromeda Galaxy|Andromeda Galaxy]]
|-


|-
|[[Astronomy:Westerlund 1-26|Westerlund 1-26]]||1,165–1,221<ref name=paulo2018 />
| L/T<sub>eff</sub>|| Very uncertain parameters for an unusual star with strong radio emission. The spectrum is variable but apparently the luminosity is not.



|-
|W60 B90 ''(WOH S264)''
|1,149<ref name="Groenewegen" />–2,555<ref name="ren" />
|L/T<sub>eff</sub>
|Located in the [[Astronomy:Large Magellanic Cloud|Large Magellanic Cloud]]
|-


|-
|HD 62745
|1,145<ref name="cruzalebes" />
|AD
|
|-


|-
|LGGS J004047.22+404445.5
|1,140<ref name="massey2016" />–1,379<ref name="gordon" />
|L/T<sub>eff</sub>
|Located in the [[Astronomy:Andromeda Galaxy|Andromeda Galaxy]]
|-
|LGGS J004035.08+404522.3
|1,140<ref name="massey2016" />–1,354<ref name="gordon" />
|L/T<sub>eff</sub>
|Located in the [[Astronomy:Andromeda Galaxy|Andromeda Galaxy]]
|-


|-
|[[Astronomy:MY Cephei|MY Cephei]]
|1,134<ref name=beasor />–2,061<ref name="massloss2020" />
|L/T<sub>eff</sub>
|Not to be confused with Mu Cephei (see below). Older estimates have given up to {{solar radius|2,440}} based on much cooler temperatures.<ref name="fawley" />
|-


|-
|LGGS J004124.80+411634.7
|1,130<ref name="massey2016" />–1,423<ref name="gordon" />
|L/T<sub>eff</sub>
|Located in the [[Astronomy:Andromeda Galaxy|Andromeda Galaxy]]
|-






|-
|ST Cephei
|1,109<ref name="cruzalebes" />
|AD
|
|-


|-
|HD 102115
|1,100<ref name="cruzalebes" />
|AD
|
|-
|LGGS J004107.11+411635.6
|1,100<ref name="massey2016" />–1,207<ref name="gordon" />
|L/T<sub>eff</sub>
|Located in the [[Astronomy:Andromeda Galaxy|Andromeda Galaxy]]
|-






|-
|LGGS J004031.00+404311.1
|1,080<ref name="massey2016" />–1,383<ref name="gordon" />
|L/T<sub>eff</sub>
|Located in the [[Astronomy:Andromeda Galaxy|Andromeda Galaxy]]
|-
|V366 Andromedae
|1,076<ref name="cruzalebes" />
|AD
|
|-


|-
|[[Astronomy:Trumpler 27-1|Trumpler 27-1]]
|1,073<ref name="messineo2019" />
|L/T<sub>eff</sub>
|Located in the massive possible [[Astronomy:Open cluster|open cluster]] [[Astronomy:Trumpler 27|Trumpler 27]]
|-





|-
|LGGS J004531.13+414825.7
|1,070<ref name="massey2016" />–1,420<ref name="gordon" />
|L/T<sub>eff</sub>
|Located in the [[Astronomy:Andromeda Galaxy|Andromeda Galaxy]]
|-
|IM Cassiopeiae
|1,068<ref name="cruzalebes" />
|AD
|
|-style="background:#F0B9AD;" class="sortbottom"
| Orbit of Jupiter || 1,064–1,173 ||  || <small>Reported for reference</small>



|-
|[[Astronomy:HR 5171|HR 5171 Aa]] (V766 Centauri Aa)
|1,060–1,160<ref name="van" />
|L/T<sub>eff</sub>
|
|-








|-
|SU Persei
|1,048<ref name="cruzalebes" />
|AD
|






{{List of largest stars row|star_name=V358 Cassiopeiae|mas=2.651194|kpc=3.658983|ref=<ref name="jsdc" />|notes=A red hypergiant star in the constellation of [[Astronomy:Cassiopeia (constellation)|Cassiopeia]].}}<ref name="Mcdonald2012" />


|-
|LGGS J004114.18+403759.8
|1,040<ref name="massey2016" />–1,249<ref name="gordon" />
|L/T<sub>eff</sub>
|Located in the [[Astronomy:Andromeda Galaxy|Andromeda Galaxy]]
|-




|-
|-
|AS Cephei
|1,026<ref name="cruzalebes" />
|AD
|
|-



|-
|LGGS J004125.72+411212.7
|1,020<ref name="massey2016" />–1,359<ref name="gordon" />
|L/T<sub>eff</sub>
|Located in the [[Astronomy:Andromeda Galaxy|Andromeda Galaxy]]
|-
|LGGS J004059.50+404542.6
|1,020<ref name="massey2016" />–1,367<ref name="gordon" />
|L/T<sub>eff</sub>
|Located in the [[Astronomy:Andromeda Galaxy|Andromeda Galaxy]]
|-


|-
|HD 167861
|1,016<ref name="cruzalebes" />
|AD
|
|-



|-
|HV 986 ''(WOH S368)''
|1,010<ref name="Levesque2007" />
|L/T<sub>eff</sub>
|Located in the [[Astronomy:Large Magellanic Cloud|Large Magellanic Cloud]]
|-


|-
! colspan="4" | The following stars with sizes below 1,000 solar radii are shown for comparison.
|-
|CZ Hydrae
|986<ref name=":1" />
|L/T<sub>eff</sub>
|One of the coolest stars at 2000 K.<ref name=":1" />
|-
|[[Astronomy:Mu Cephei|Mu Cephei]] ''(Herschel's "Garnet Star")''
|972 ± 228<ref name="montarges2019" />
|L/T<sub>eff</sub>
|Prototype of the obsolete class of the Mu Cephei variables and also one of reddest stars in the night sky in terms of the B-V color index.<ref name="groups.google.com" /> Other estimates have given as high as {{solar radius|1,650}} based on angular diameter.<ref name="kaler" />
|-
|[[Astronomy:V602 Carinae|V602 Carinae]]
|932<ref name="messineo2019" />–1,151<ref name="cruzalebes" />
|AD
|
|-
| [[Astronomy:Betelgeuse|Betelgeuse]] ''(Alpha Orionis)'' || {{val|764|116|62}}<ref name="joyce2020" /> || AD || Star with the third largest apparent size after R Doradus and the Sun. Brightest red supergiant in the night sky. Another estimate gives {{val|955|217|u={{solar radius}}}}<ref name="NEILSON2011" />
|-
|[[Astronomy:Antares|Antares A]] ''(Alpha Scorpii A)''|| 707<ref name="cruzalebes" /> || AD || Antares was originally calculated to be over {{Solar radius|850}},<ref name="Pugh2013" /><ref name="Baade2007" /> but those estimates are likely to have been affected by asymmetry of the atmosphere of the star.<ref name="ohnaka2013" />
|-
| [[Astronomy:V354 Cephei|V354 Cephei]] || 685<ref name="messineo2019" /> || L/T<sub>eff</sub> ||
|-
|[[Astronomy:KY Cygni|KY Cygni]]
|672<ref name="messineo2019" />–1,420<ref name="levesqueetal2005" /><ref name=trevor />
|L/T<sub>eff</sub>
|
|-style="background:#afeeee;" class="sortbottom"
| [[Astronomy:Ceres (dwarf planet)#Orbit|Orbit of Ceres]] || [[Astronomy:Astronomical unit|595]] (550–641)|| || <small>Reported for reference</small>
|-
|[[Astronomy:119 Tauri|119 Tauri]] ''(CE Tauri)''|| 587–593<ref name="montarges2018" /> || AD || <!--Second reddest star in the night sky.<ref name="groups.google.com" />-->Can be occulted by the Moon, allowing accurate determination of its apparent diameter.
|-
|[[Astronomy:CW Leonis|CW Leonis]] || 580–686<ref name="schmidt" /> || L/T<sub>eff</sub> || Prototype of [[Astronomy:Carbon star|carbon star]]s. CW Leo was mistakenly identified as the claimed planet "[[Unsolved:Nibiru cataclysm|Nibiru]]" or "[[Astronomy:Planet X|Planet X]]".
|-
|[[Astronomy:Mira|Mira A]] ''(Omicron Ceti)'' || 541<ref name="debeck" /> || AD || Prototype [[Astronomy:Mira variable|Mira variable]]. De beck ''et al.'' 2010 calculates {{solar radius|541}}.<ref name="debeck" />
|-
|[[Astronomy:VV Cephei|VV Cephei A]] || 516<ref name="tess" />–1,000<ref name="pollmann" /> ||EB
|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. Data from the most recent eclipse has cast additional doubt on the accepted model of the system. Older estimates give up to {{solar radius|1,900}}<ref name="levesqueetal2005" />
|-
|[[Astronomy:V382 Carinae|V382 Carinae]] ''(x Carinae)''|| 485 ± 40<ref name="cepheids" />||AD
|[[Astronomy:Yellow hypergiant|Yellow hypergiant]], one of the rarest types of a star.
|-
|[[Astronomy:Pistol Star|Pistol Star]]|| 435<ref name="ryan" /> || AD || Blue [[Astronomy:Hypergiant|hypergiant]], among the most massive and luminous stars known.
|-
| [[Astronomy:HD 179821|HD 179821]] || 400–450<ref name="van" />
|DSKE
|V1427 Aquilae may be a [[Astronomy:Yellow hypergiant|yellow hypergiant]] or a much less luminous star.
|-
|[[Astronomy:V509 Cassiopeiae|V509 Cassiopeiae]] || 390–910<ref name="hr8752">{{cite journal|doi=10.1051/0004-6361/201117166|title=The hypergiant HR 8752 evolving through the yellow evolutionary void|journal=Astronomy & Astrophysics|volume=546|pages=A105|year=2012|last1=Nieuwenhuijzen|first1=H.|last2=De Jager|first2=C.|last3=Kolka|first3=I.|last4=Israelian|first4=G.|last5=Lobel|first5=A.|last6=Zsoldos|first6=E.|last7=Maeder|first7=A.|last8=Meynet|first8=G.|bibcode=2012A&A...546A.105N|url=http://www.vliz.be/imisdocs/publications/72/262672.pdf|doi-access=free}}</ref>|| AD ||[[Astronomy:Yellow hypergiant|Yellow hypergiant]], one of the rarest types of a star.
|-style="background:#EEEEEE;" class="sortbottom"
| Inner limits of the [[Astronomy:Asteroid belt|asteroid belt]] || 380 || || <small>Reported for reference</small>
|-
|[[Astronomy:IRC +10420|IRC +10420]] || 380<ref name="wong">{{cite journal|arxiv=1710.01027|doi=10.1051/0004-6361/201731873|title=Circumstellar ammonia in oxygen-rich evolved stars|year=2018|last1=Wong|first1=K. T.|last2=Menten|first2=K. M.|last3=Kamiński|first3=T.|last4=Wyrowski|first4=F.|last5=Lacy|first5=J. H.|last6=Greathouse|first6=T. K.|journal=Astronomy & Astrophysics|volume=612|pages=A48|bibcode=2018A&A...612A..48W|s2cid=55019902}}</ref>|| L/T<sub>eff</sub> || A [[Astronomy:Yellow hypergiant|yellow hypergiant]] that has increased its temperature into the [[Astronomy:Luminous blue variable|LBV]] range. De beck ''et al.'' 2010 calculates {{solar radius|1,342}} based on a much cooler temperature.<ref name=debeck/>
|-
|V688 Monocerotis
|372<ref name=":1" />
|L/T<sub>eff</sub>
|Also one of the coolest stars at 2000 K.<ref name=":1" />
|-
|[[Astronomy:R Doradus|R Doradus]]||298 ± 21<ref>{{cite journal|last1=Ohnaka|first1=Keiichi|last2=Weigelt|first2=Gerd|last3=Hofmann|first3=Karl-Heinz|year=2019|title=Infrared Interferometric Three-dimensional Diagnosis of the Atmospheric Dynamics of the AGB Star R Dor with VLTI/AMBER|journal=The Astrophysical Journal|volume=883|issue=1|pages=89|arxiv=1908.06997|bibcode=2019ApJ...883...89O|doi=10.3847/1538-4357/ab3d2a|s2cid=201103617}}</ref>||AD
| Star with the second largest apparent size after the Sun.
|-style="background:#E3A1A1" class="sortbottom"
| [[Astronomy:Orbit of Mars|Orbit of Mars]]|| 297–358 ||  || <small>Reported for reference</small>
|-
|[[Astronomy:La Superba|La Superba]] ''(Y Canum Venaticorum)''|| 289<ref name="cruzalebes" />–352<ref>{{cite arXiv|eprint=1808.01439|last1=Tram|first1=L. N.|last2=Lesaffre|first2=P.|last3=Cabrit|first3=S.|last4=Nhung|first4=P. T.|title=Bow-shock chemistry in the interstellar medium|year=2018|class=astro-ph.SR}}</ref>|| AD and L/T<sub>eff</sub> || Referred to as ''La Superba'' by Angelo Secchi. Currently one of the [[Astronomy:List of coolest stars|coolest]] and reddest stars.
|-style="background:pink;" class="sortbottom"
| Sun's red giant phase || 256<ref>{{cite journal | author = Rybicki, K. R. | author2 = Denis, C. | title = On the Final Destiny of the Earth and the Solar System | journal = Icarus | volume = 151 | issue = 1 | pages = 130–137 | date = 2001 | doi = 10.1006/icar.2001.6591 | bibcode = 2001Icar..151..130R}}</ref>|| || At this point, the Sun will engulf [[Astronomy:Mercury (planet)|Mercury]] and [[Astronomy:Venus|Venus]], and possibly the [[Astronomy:Earth|Earth]] although it will move away from its orbit since the Sun will lose a third of its mass. During the helium burning phase, it will shrink to {{solar radius|10}} but will later grow again and become an unstable AGB star, and then a white dwarf after making a [[Astronomy:Planetary nebula|planetary nebula]].<ref>{{Cite journal | last1 = Schröder | first1 = K.-P. | last2 = Connon Smith | first2 = R. | doi = 10.1111/j.1365-2966.2008.13022.x | title = Distant future of the Sun and Earth revisited | journal = Monthly Notices of the Royal Astronomical Society | volume = 386 | issue = 1 | pages = 155–163 | year = 2008 |arxiv = 0801.4031 |bibcode = 2008MNRAS.386..155S | s2cid = 10073988}}</ref><ref>{{Cite journal | last1 = Vassiliadis | first1 = E. | last2 = Wood | first2 = P.R. | doi = 10.1086/173033 | title = Evolution of low- and intermediate-mass stars to the end of the asymptotic giant branch with mass loss | journal = The Astrophysical Journal | volume = 413 | page = 641 | year = 1993 |bibcode = 1993ApJ...413..641V}}</ref> <small>Reported for reference</small>
|-
|[[Astronomy:Rho Cassiopeiae|Rho Cassiopeiae]]|| 242<ref name="cruzalebes" />|| AD ||[[Astronomy:Yellow hypergiant|Yellow hypergiant]], one of the rarest types of a star.
|-
|[[Astronomy:Eta Carinae|Eta Carinae A]] || ~240<ref>{{Cite journal | last1 = Gull | first1 = T. R. | last2 = Damineli | first2 = A. | doi =10.1017/S1743921310009890 | title = JD13 – Eta Carinae in the Context of the Most Massive Stars | journal = Proceedings of the International Astronomical Union | volume = 5 | pages = 373–398 | year = 2010 |arxiv = 0910.3158 |bibcode = 2010HiA....15..373G | s2cid = 1845338}}</ref>|| || Previously thought to be the most massive single star, but in 2005 it was realized to be a binary system. During the Great Eruption, the size was much larger at around {{solar radius|1,400}}.<ref>{{cite journal |bibcode=2011MNRAS.415.2020S|title=Explosions triggered by violent binary-star collisions: Application to Eta Carinae and other eruptive transients|journal=Monthly Notices of the Royal Astronomical Society|volume=415|issue=3|pages=2020–2024|last1=Smith|first1=Nathan|year=2011|doi=10.1111/j.1365-2966.2011.18607.x|arxiv = 1010.3770 |s2cid=119202050}}</ref> η Car is calculated to be between {{solar radius|60}} and {{solar radius|881}}.<ref>{{cite journal |author=D. John Hillier |author2=K. Davidson |author3=K. Ishibashi |author4=T. Gull |title=On the Nature of the Central Source in η Carinae |journal=Astrophysical Journal |volume=553 |issue=837 |pages=837 |date=June 2001 |bibcode=2001ApJ...553..837H |doi=10.1086/320948|doi-access=free }}</ref>
|-style="background:#ADD8E6;" class="sortbottom"
| Orbit of Earth || [[Astronomy:Astronomical unit|215]](211–219)|| || <small>Reported for reference</small>
|- style="background:#A3FFA3;" class="sortbottom"
| Solar System Habitable Zone || 200–520<ref>{{cite journal |title=A Volcanic Hydrogen Habitable Zone |last1=Ramirez |first1=Ramses |date=2017 |arxiv=1702.08618|last2=Kaltenegger |first2=Lisa |doi=10.3847/2041-8213/aa60c8 |volume=837 |issue=1 |pages=L4 |journal=The Astrophysical Journal Letters|bibcode=2017ApJ...837L...4R|s2cid=119333468}}</ref> (uncertain) || || <small>Reported for reference</small>
|-style="background:Gold;" class="sortbottom"
| [[Astronomy:Orbit of Venus|Orbit of Venus]] || 154–157 ||  || <small>Reported for reference</small>
|-
|[[Astronomy:Epsilon Aurigae|Epsilon Aurigae]] A ''(Almaaz A)'' || 143–358<ref>{{cite journal |bibcode=2015ApJS..220...14K |arxiv=1508.01909 |title=Interferometry of ɛ Aurigae: Characterization of the Asymmetric Eclipsing Disk |journal=The Astrophysical Journal Supplement Series |volume=220 |issue=1 |pages=14 |last1=Kloppenborg|first1=B.K. |last2=Stencel|first2=R.E. |last3=Monnier|first3=J.D. |last4=Schaefer|first4=G.H. |last5=Baron|first5=F. |last6=Tycner|first6=C. |last7=Zavala|first7=R.T. |last8=Hutter|first8=D. |last9=Zhao|first9=M. |last10=Che|first10=X. |last11=Ten Brummelaar |first11=T.A. |last12=Farrington|first12=C.D. |last13=Parks|first13=R. |last14=McAlister|first14=H. A. |last15=Sturmann|first15=J. |last16=Sturmann|first16=L. |last17=Sallave-Goldfinger|first17=P.J. |last18=Turner|first18=N. |last19=Pedretti|first19=E. |last20=Thureau|first20=N. |year=2015 |doi=10.1088/0067-0049/220/1/14|s2cid=118575419}}</ref>|| AD || ε Aurigae was incorrectly claimed in 1970 as the largest star with a size between {{solar radius|2,000}} and {{solar radius|3,000}},<ref>{{cite web |url=https://news.google.com/newspapers?id=rcgyAAAAIBAJ&pg=793,4107018 |title=Ask Andy: The Biggest Star |work=Ottawa Citizen |page=23 |date=Nov 27, 1970}}</ref> even though it later turned out not to be an ''infrared light star'' but rather a dusk torus surrounding the system.
|-
|[[Astronomy:Deneb|Deneb]] ''(Alpha Cygni)''|| 99.84<ref name="cruzalebes" />|| AD || Prototype [[Astronomy:Alpha Cygni variable|Alpha Cygni variable]].
|-
| [[Astronomy:WR 102ka|Peony Star]] || 92<ref>{{Cite journal | last1 = Barniske | first1 = A. | last2 = Oskinova | first2 = L. M. | last3 = Hamann | first3 = W. -R. | doi = 10.1051/0004-6361:200809568 | title = Two extremely luminous WN stars in the Galactic center with circumstellar emission from dust and gas | journal = Astronomy and Astrophysics | volume = 486 | issue = 3 | pages = 971 | year = 2008 |arxiv = 0807.2476 |bibcode = 2008A&A...486..971B | s2cid = 8074261}}</ref>|| AD || Candidate for most luminous star in the [[Astronomy:Milky Way|Milky Way]].
|-
| [[Astronomy:Canopus|Canopus]] ''(Alpha Carinae)'' || 71<ref>{{cite journal|last1=Cruzalebes|first1=P.|last2=Jorissen|first2=A.|last3=Rabbia|first3=Y.|last4=Sacuto|first4=S.|last5=Chiavassa|first5=A.|last6=Pasquato|first6=E.|last7=Plez|first7=B.|last8=Eriksson|first8=K.|last9=Spang|first9=A.|last10=Chesneau|first10=O.|title=Fundamental parameters of 16 late-type stars derived from their angular diameter measured with VLTI/AMBER|journal=Monthly Notices of the Royal Astronomical Society|volume=434|issue=1|year=2013|pages=437–450 |doi=10.1093/mnras/stt1037 |bibcode=2013MNRAS.434..437C|arxiv = 1306.3288 |s2cid=49573767}}</ref>|| AD || [[Astronomy:List of brightest stars|Second brightest star]] in the night sky.
|-style="background:#d3d3d3;" class="sortbottom"
| Orbit of Mercury || 66–100 ||  || <small>Reported for reference</small>
|-
| [[Astronomy:LBV 1806-20|LBV 1806-20]] || 46–145<ref>{{cite journal|doi=10.1086/422180|title=Infrared Observations of the Candidate LBV 1806‐20 and Nearby Cluster Stars|journal=The Astrophysical Journal|volume=616|issue=1|pages=506–518|year=2004|last1=Eikenberry|first1=S. S.|last2=Matthews|first2=K.|last3=Lavine|first3=J. L.|last4=Garske|first4=M. A.|last5=Hu|first5=D.|last6=Jackson|first6=M. A.|last7=Patel|first7=S. G.|last8=Barry|first8=D. J.|last9=Colonno|first9=M. R.|last10=Houck|first10=J. R.|last11=Wilson|first11=J. C.|last12=Corbel|first12=S.|last13=Smith|first13=J. D.|bibcode=2004ApJ...616..506E|arxiv = astro-ph/0404435 |s2cid=18042381}}</ref>|| L/T<sub>eff</sub> || Formerly a candidate for the most luminous star in the [[Astronomy:Milky Way|Milky Way]] with {{solar luminosity|40 million}},<ref>{{cite web |first=Meghan |last=Kennedy |url=http://www.solstation.com/x-objects/1806-20.htm |title=LBV 1806-20 AB? |website=SolStation.com |access-date=2017-10-28 |archive-url=https://web.archive.org/web/20171113031139/http://www.solstation.com/x-objects/1806-20.htm |archive-date=2017-11-13 |url-status=live}}</ref> but the luminosity has been revised later only {{solar luminosity|2 million}}.<ref>{{Cite journal | last1 = Figer | first1 = D. F. | last2 = Najarro | first2 = F. | last3 = Kudritzki | first3 = R. P. | doi = 10.1086/423306 | title = The Double-lined Spectrum of LBV 1806-20 | journal = The Astrophysical Journal | volume = 610 | issue = 2 | pages = L109–L112 | year = 2004 |arxiv = astro-ph/0406316 |bibcode = 2004ApJ...610L.109F | s2cid = 118975170}}</ref><ref>{{cite journal|doi=10.1051/0004-6361/201118040|title=The first X-ray survey of Galactic luminous blue variables |journal=Astronomy & Astrophysics |volume=538 |issue=47 |pages=A47 |year=2012 |last1=Nazé |first1=Y. |last2=Rauw |first2=G. |last3=Hutsemékers |first3=D. |bibcode= 2012A&A...538A..47N |arxiv = 1111.6375 |s2cid=43688343}}</ref>
|-
| [[Astronomy:Aldebaran|Aldebaran]] ''(Alpha Tauri)'' || 44.13 ± 0.84<ref>{{cite journal | bibcode=2018ApJ...865L..20F | title=Aldebaran b's Temperate Past Uncovered in Planet Search Data | journal=The Astrophysical Journal | volume=865 | issue=2 | pages=L20 | last1=Farr | first1=Will M. | last2=Pope | first2=Benjamin J. S. | last3=Davies | first3=Guy R. | last4=North | first4=Thomas S. H. | last5=White | first5=Timothy R. | last6=Barrett | first6=Jim W. | last7=Miglio | first7=Andrea | last8=Lund | first8=Mikkel N. | last9=Antoci | first9=Victoria | last10=Fredslund Andersen | first10=Mads | last11=Grundahl | first11=Frank | last12=Huber | first12=Daniel | year=2018 | doi=10.3847/2041-8213/aadfde | arxiv=1802.09812 | s2cid=56049041 | url=http://pure-oai.bham.ac.uk/ws/files/54771082/Farr_2018_ApJL_865_L20.pdf | access-date=2019-12-16 | archive-url=https://web.archive.org/web/20200303134958/http://pure-oai.bham.ac.uk/ws/files/54771082/Farr_2018_ApJL_865_L20.pdf | archive-date=2020-03-03 | url-status=dead}}</ref>|| AD || [[Astronomy:List of brightest stars|Fourteenth brightest star]] in the night sky
|-
| [[Astronomy:R136a1|R136a1]] || 39.2<ref>{{cite journal |bibcode=2020MNRAS.499.1918B |title=The R136 star cluster dissected with Hubble Space Telescope/STIS. II. Physical properties of the most massive stars in R136 |last1=Bestenlehner |first1=Joachim M. |last2=Crowther |first2=Paul A. |last3=Caballero-Nieves |first3=Saida M. |last4=Schneider |first4=Fabian R. N. |last5=Simón-Díaz |first5=Sergio |last6=Brands |first6=Sarah A. |last7=De Koter |first7=Alex |last8=Gräfener |first8=Götz |last9=Herrero |first9=Artemio |last10=Langer |first10=Norbert |last11=Lennon |first11=Daniel J. |last12=Maíz Apellániz |first12=Jesus |last13=Puls |first13=Joachim |last14=Vink |first14=Jorick S. |journal=Monthly Notices of the Royal Astronomical Society |year=2020 |volume=499 |issue=2 |page=1918 |doi=10.1093/mnras/staa2801 |arxiv=2009.05136|s2cid=221640940 }}</ref>|| L/T<sub>eff</sub> || Also on record as one of the most massive and luminous stars known ({{solar mass|215}} and {{solar luminosity|6.2 million}}).
|-
| [[Astronomy:Polaris|Polaris]] ''(Alpha Ursae Minoris)'' ||37.5<ref>{{cite journal|bibcode=2015MNRAS.449.1011F |arxiv=1502.06463|doi = 10.1093/mnras/stv412 |title=Evolutionary status of Polaris|journal=Monthly Notices of the Royal Astronomical Society|volume=449|issue=1|pages=1011–1017|year=2015|last1=Fadeyev|first1=Y. A.|s2cid=118517157}}</ref>|| AD || The current northern [[Astronomy:Pole star|pole star]].
|-
| [[Astronomy:Arcturus|Arcturus]] ''(Alpha Boötis)'' || 24.25<ref name="cruzalebes" />|| AD || Brightest star in the [[Astronomy:Northern celestial hemisphere|northern celestial hemisphere]].
|-
| [[Astronomy:Cygnus X-1|HDE 226868]] || 20–22<ref>{{cite journal | last=Ziółkowski | first=J. | title=Evolutionary constraints on the masses of the components of HDE&nbsp;226868/Cyg&nbsp;X-1 binary system | journal=Monthly Notices of the Royal Astronomical Society | date=2005 | volume=358 | issue=3 | pages=851–859 | arxiv=astro-ph/0501102 | doi=10.1111/j.1365-2966.2005.08796.x | bibcode=2005MNRAS.358..851Z| s2cid=119334761}} Note: For radius, see Table 1 with ''d''=2&nbsp;kpc.</ref>|| || The supergiant companion of black hole Cygnus X-1. The black hole is around 500,000 times smaller than the star.
|-style="background:pink;" class="sortbottom"
| [[Astronomy:Sun|Sun]] || 1 || || The largest object in the [[Astronomy:Solar System|Solar System]].<br /><small>Reported for reference</small>
|}

{{notelist}}

==See also==
{{cmn|
* [[Astronomy:Constellation|Constellation]]
* [[Astronomy:Lists of stars|Lists of stars]]
* [[Astronomy:List of most massive stars|List of most massive stars]]
* [[Astronomy:List of most luminous stars|List of most luminous stars]]
* [[Astronomy:List of hottest stars|List of hottest stars]]
* [[Astronomy:List of coolest stars|List of coolest stars]]
* [[Astronomy:List of most massive black holes|List of most massive black holes]]
* [[Astronomy:List of largest nebulae|List of largest nebulae]]
* [[Astronomy:List of largest galaxies|List of largest galaxies]]
* [[Astronomy:List of largest cosmic structures|List of largest cosmic structures]]
* [[Astronomy:List of largest exoplanets|List of largest exoplanets]]
* [[Astronomy:List of star extremes|List of star extremes]]
* [[Astronomy:Star|Star]]
}}

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}}

==External links==
* [https://web.archive.org/web/20150419074502/http://www.giant-stars.de/ Giant Stars] An interactive website comparing the Earth and the Sun to some of the largest known stars
* [http://news.bbc.co.uk/2/hi/science/nature/4164365.stm Three largest stars identified] BBC News
* [http://www.universetoday.com/2008/04/06/what-is-the-biggest-star-in-the-universe/ What is the Biggest Star in the Universe?] Universe Today

{{Star}}
{{DEFAULTSORT:Largest stars, List of}}
[[Category:Hypergiants]]
[[Category:Supergiants]]
[[Category:Lists of stars|Largest]]
[[Category:Lists of superlatives in astronomy|Stars, largest]]

{{Sourceattribution|List of largest stars|1}}