User:Ynoss/sandbox
This is Ynoss's sandbox. Please do not do any <<damage>> to it. You may edit it, but do not vandalize it or you may be blocked from editing! BTW, I am not an admin but later in the future. Thank you—Ynoss THE OFFICIAL ★ ✉ discussion / CONTRIBS 08:18, 16 July 2017 (UTC)
This is a '''list of largest objects in the universe'''. [[Black holes]], [[nebulae]], [[galaxies]], [[superclusters]], [[Void (astronomy)|voids]] and [[galaxy filament]]s are not included, but to give you a perspective of how big things can get, here is a reference point:
[[Hercules–Corona Borealis Great Wall]], the [[List of largest cosmic structures|largest known structure]], is 6,000,000,000 × 10,000,000,000 [[light years]]
[[KBC Void]] (larger than the [[Giant Void]]), the [[List of largest voids|largest known void]], is 2,000,000,000 [[light years]]
[[List of largest cosmic structures|Caelum Supercluster]], the [[list of largest cosmic structures|largest known supercluster]], is 910,000,000 [[light years]]
[[IC 1101]], the [[List of largest galaxies|largest known galaxy]], is 5,500,000 × 6,600,000 [[light years]] in diameter.
[[NGC 604]], the [[list of largest nebulae|largest known nebula]], is 1,520 [[light years]] in diameter.
[[S5 0014+81]], the [[List of most massive black holes|most massive black hole known]], is 40 billion [[solar mass]]es which is equal to 1,582 [[astronomical units]].
[[L1551 IRS 5]] is *'''not'''* 10,600 solar radii because, its size is not '''confirmed''' ''(Its size is probably '''0.212 solar radii''')'', because of his '''age'''.
*As the Earth, due to collisions with asteroids, the Earth's radius has '''decreased'''.
*As the Sun too, due to formation, the Sun's radius has '''decreased''' as the Earth.
:''And the stellar evolutionary theory limit is only '''2,000 (or 3,000) solar radii''' so, L 1551 IRS5's size can be no larger than 3,000 solar radii.''
''And also Shadron Soul and VY Masses Majoris '''don't exist'''.''
=<!--==-->=
{{distinguish|List of most massive stars}}
[[File:Comparison of planets and stars (sheet by sheet) (Apr 2015 update).png|thumb|500px|Relative sizes of the [[planets]] in the [[Solar System]] and some of the largest [[stars]]:
{{ordered list
| [[Mercury (planet)|Mercury]] < [[Mars]] < [[Venus]] < [[Earth]]
| [[Earth]] < [[Neptune]] < [[Uranus]] < [[Saturn]] < [[Jupiter]]
| [[Jupiter]] < [[Proxima Centauri]] < [[Sun]] < [[Sirius]]
| [[Sirius]] < [[Pollux (star)|Pollux]] < [[Arcturus]] < [[Aldebaran]]
| [[Aldebaran]] < [[Rigel]] < [[Antares]] < [[Betelgeuse]]
| [[Betelgeuse]] < [[VY Canis Majoris]] < [[NML Cygni]] < [[UY Scuti]]
}}]]
Below is a '''list of the largest stars''' so far discovered, ordered by [[radius]]. The unit of measurement used is the [[Solar radius|radius of the Sun]] ({{convert|1|solar radius|km mi|0|abbr=on|disp=out}}).
==Caveats==
[[File:UY Scuti zoomed in, Rutherford Observatory, 07 September 2014.jpeg|thumb|left||[[UY Scuti]] as seen in visible light.]]
The exact order of this list is not complete, nor is it perfectly defined:
*There are sometimes high uncertainties in derived values and sizes;
*The distances to most of these [[star]]s are uncertain to differing degrees and this uncertainty affects the size measurements;
*All the stars in this list have extended atmospheres, many are embedded in mostly opaque dust shells or disks, and most pulsate, such that their radii are not well defined;
*There are theoretical reasons for expecting that no stars in the [[Milky Way]] are larger than approximately 2,600 times the Sun (roughly 3,715 K and M<sub>bol</sub> = −9), based on [[stellar evolution|evolutionary models]]. The exact limit depends on the [[metallicity]] of the star, so for example [[supergiant]]s in the [[Magellanic Clouds]] have slightly different limiting [[effective temperature|temperature]] and [[bolometric luminosity|luminosity]]. Stars exceeding the limit have been seen to undergo large eruptions and to change their [[spectral type]] over just a few months;<ref name=levesqueetal2005 />
*A survey of the Magellanic Clouds has catalogued most of the [[red supergiant]]s and 50 of them are larger than the {{convert|700|solar radius|km AU mi|abbr=on|lk=on|}} cutoff point of this table, with the largest at 1,200–1,300.<ref name=mc>{{Cite journal |author1-link=Emily Levesque | last1 = Levesque | first1 = E. M. | last2 = Massey | first2 = P. | last3 = Olsen | first3 = K. A. G. | last4 = Plez | first4 = B. | last5 = Meynet | first5 = G. | last6 = Maeder | first6 = A. | doi = 10.1086/504417 | title = The Effective Temperatures and Physical Properties of Magellanic Cloud Red Supergiants: The Effects of Metallicity | journal = The Astrophysical Journal | volume = 645 | issue = 2 | pages = 1102 | year = 2006 | pmid = | pmc = |arxiv = astro-ph/0603596 |bibcode = 2006ApJ...645.1102L }}</ref>
{{clear}}
==List==
{| class="wikitable sortable"
|+'''List of the largest stars'''
|-
! style="background:#efefef; white-space:nobr;width:13.375em"| Star name
! style="background-color:#FFDEAD;" | [[Solar radius|Solar radii]]<br/>([[Sun]] = 1)
! Notes
|-
|[[UY Scuti]] || 1,708 ± 192<ref name="torres2013">{{Cite journal | last1 = Arroyo-Torres | first1 = B. | last2 = Wittkowski | first2 = M. | last3 = Marcaide | first3 = J. M. | last4 = Hauschildt | first4 = P. H. | title = The atmospheric structure and fundamental parameters of the red supergiants AH Scorpii, UY Scuti, and KW Sagittarii | doi = 10.1051/0004-6361/201220920 | journal = Astronomy & Astrophysics | volume = 554 | pages = A76 | year = 2013 | pmid = | pmc = | bibcode = 2013A&A...554A..76A |arxiv = 1305.6179 }}</ref> || [[Margin of error]] in size determination: ± 192 solar radii. At its smallest, its size would be similar to that of V354 Cephei (see below).
|-<!--
| [[NML Cygni]] || 1,650<ref name=zhang/> ||
|--->
| [[WOH G64]] || 1,540<ref name="Levesque2009">
{{cite journal
|title=The Physical Properties of the Red Supergiant WOH G64: The Largest Star Known?
|journal=Astronomical Journal
|author=Emily M. Levesque, Philip Massey, Bertrand Plez, and Knut A. G. Olsen
|volume=137 |issue=6 |pages=4744
|date=June 2009
|bibcode=2009AJ....137.4744L
|doi=10.1088/0004-6256/137/6/4744
}}</ref>–1,730<ref name=ohnaka>{{Cite journal | last1 = Ohnaka | first1 = K. | last2 = Driebe | first2 = T. | last3 = Hofmann | first3 = K. H. | last4 = Weigelt | first4 = G. | last5 = Wittkowski | first5 = M. | title = Resolving the dusty torus and the mystery surrounding LMC red supergiant WOH G64 | doi = 10.1017/S1743921308028858 | journal = Proceedings of the International Astronomical Union | volume = 4 | pages = 454 | year = 2009 | pmid = | pmc = | bibcode = 2009IAUS..256..454O }}</ref> || This would be the largest star in the [[Large Magellanic Cloud|LMC]], but is unusual in position and motion and might still be a foreground halo giant. [[Margin of error|Margin of possible error]]: ± 77 solar radii (Levesque 2009).
|-
| [[RW Cephei]] || {{nobr| 1,535<ref name=humphreys>{{cite journal|doi=10.1086/190559|title=Studies of luminous stars in nearby galaxies. I. Supergiants and O stars in the Milky Way|journal=The Astrophysical Journal Supplement Series|volume=38|pages=309|year=1978|last1=Humphreys|first1=R. M.|bibcode=1978ApJS...38..309H}}</ref><ref name=davies>{{cite journal|doi=10.1111/j.1365-2966.2010.16965.x|title=The potential of red supergiants as extragalactic abundance probes at low spectral resolution|journal=Monthly Notices of the Royal Astronomical Society|volume=407|issue=2|pages=1203|year=2010|last1=Davies|first1=Ben|last2=Kudritzki|first2=Rolf-Peter|last3=Figer|first3=Donald F.|bibcode=2010MNRAS.407.1203D|arxiv = 1005.1008 }}</ref> }}({{nobr| 1,260–1,610 }} {{Citation needed|date=December 2009}}) || 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 size is just an estimate.
|-
| [[Westerlund 1-26]] || {{nobr| 1,530-1,580<ref name=wright>{{cite journal|last1=Wright|first1=N. J.|last2=Wesson|first2=R.|last3=Drew|first3=J. E.|last4=Barentsen|first4=G.|last5=Barlow|first5=M. J.|last6=Walsh|first6=J. R.|last7=Zijlstra|first7=A.|last8=Drake|first8=J. J.|last9=Eisloffel|first9=J.|last10=Farnhill|first10=H. J.|title=The ionized nebula surrounding the red supergiant W26 in Westerlund 1|journal=Monthly Notices of the Royal Astronomical Society: Letters|date=16 October 2013|volume=437|issue=1|pages=L1–L5|doi=10.1093/mnrasl/slt127|arxiv = 1309.4086 |bibcode = 2014MNRAS.437L...1W }}</ref> (–2,544)}}<ref name=clark>{{cite journal|doi=10.1051/0004-6361/201116990|title=A VLT/FLAMES survey for massive binaries in Westerlund 1|journal=Astronomy & Astrophysics|volume=531|pages=A28|year=2011|last1=Clark|first1=J. S.|last2=Ritchie|first2=B. W.|last3=Negueruela|first3=I.|last4=Crowther|first4=P. A.|last5=Damineli|first5=A.|last6=Jablonski|first6=F. J.|last7=Langer|first7=N.}}</ref><ref>{{cite journal|doi=10.1051/0004-6361/200913820|title=A serendipitous survey for variability amongst the massive stellar population of Westerlund 1|journal=Astronomy and Astrophysics|volume=514|pages=A87|year=2010|last1=Clark|first1=J. S.|last2=Ritchie|first2=B. W.|last3=Negueruela|first3=I.}}</ref> || Very uncertain parameters for an unusual star with strong radio emission. The spectrum is variable but apparently the luminosity is not. Clark ''et al'' estimated it to be as large as {{solar radius|1,951–2,544}}.
|-
| [[V354 Cephei]] || 690<ref name=mauron/>-1,520<ref name=levesqueetal2005 />
|-
| [[V766 Centauri|HR 5171 A]] || {{nobr| 1,490 ± 540<ref name=wittkowski2017>{{cite journal|bibcode=2017A&A...597A...9W|arxiv=1610.01927|title=VLTI/AMBER spectro-interferometry of the late-type supergiants V766 Cen (=HR 5171 A), σ Oph, BM Sco, and HD 206859|journal=Astronomy & Astrophysics|volume=597|pages=A9|author1=Wittkowski|first1=M.|last2=Arroyo-Torres|first2=B.|last3=Marcaide|first3=J. M.|last4=Abellan|first4=F. J.|last5=Chiavassa|first5=A.|last6=Guirado|first6=J. C.|year=2017|doi=10.1051/0004-6361/201629349}}</ref>}} || HR 5171 A is a highly distorted star in a close binary system, losing mass to the secondary. According to Chesneau ''et al''; it may be the largest star of its type ([[yellow hypergiant]]), but may be of early K-type class or of early M-type. In another opinion (such as Chesneau, Meilland and Chapellier) say that the star has a radius around {{solar radius|1,315 ± 260}}.<ref name="chesneau">{{cite journal|bibcode=2014A&A...563A..71C|arxiv=1401.2628v2|title=The yellow hypergiant HR 5171 A: Resolving a massive interacting binary in the common envelope phase|journal=Astronomy & Astrophysics|volume=563|pages=A71|author1=Chesneau|first1=O.|last2=Meilland|first2=A.|last3=Chapellier|first3=E.|last4=Millour|first4=F.|last5=Van Genderen|first5=A. M.|last6=Nazé|first6=Y.|last7=Smith|first7=N.|last8=Spang|first8=A.|last9=Smoker|first9=J. V.|last10=Dessart|first10=L.|last11=Kanaan|first11=S.|last12=Bendjoya|first12=Ph.|last13=Feast|first13=M. W.|last14=Groh|first14=J. H.|last15=Lobel|first15=A.|last16=Nardetto|first16=N.|last17=Otero|first17=S.|last18=Oudmaijer|first18=R. D.|last19=Tekola|first19=A. G.|last20=Whitelock|first20=P. A.|last21=Arcos|first21=C.|last22=Curé|first22=M.|last23=Vanzi|first23=L.|year=2014|doi=10.1051/0004-6361/201322421}}</ref>
|-
| [[KY Cygni]] || {{nobr| 1,420–2,850 }} <ref name=levesqueetal2005 /> || The upper estimate is due to an unusual K band measurement and thought to be an artefact of a reddening correction error. The lower estimate is consistent with other stars in the same survey and with theoretical models.
|-
| [[VY Canis Majoris]] || 1,420 || Humphreys ''et al'' originally estimated the radius of VY CMa to be at 2,252 solar radii; a size so large that places it outside the bounds of [[stellar evolution]]ary theory. The quoted size is based on an improved measurement by Wittowski ''et al''. Another study by Massey, Levesque, and Plez concludes that the star has a radius around 600-2,800 solar radii.<ref name="Choi">
{{cite journal
|title=Distance to VY VMa with VERA
|publisher=Publications Astronomical Society of Japan
|author= Y. K. Choi
|bibcode=2008PASJ...60.1007C
|author2=Hirota, Tomoya
|author3=Honma, Mareki
|author4=Kobayashi, Hideyuki
|author5=Bushimata, Takeshi
|author6=Imai, Hiroshi
|author7=Iwadate, Kenzaburo
|author8=Jike, Takaaki
|author9=Kameno, Seiji
|volume=60
|issue=5
|year=2008
|page=1007
|journal=Publications of the Astronomical Society of Japan
|last2=Hirota
|last3=Honma
|last4=Kobayashi
|last5=Bushimata
|last6=Imai
|last7=Iwadate
|last8=Jike
|last9=Kameno
|arxiv = 0808.0641 |doi=10.1093/pasj/60.5.1007
}}</ref>
|-
| [[AH Scorpii]] || {{nobr|1,287-1,535}}<ref name=torres2013/> || AH Sco is variable by nearly 3 magnitudes in the visual range, and an estimated 20% in total luminosity. The variation in diameter is not clear because the temperature also varies.
|-
| [[VV Cephei|VV Cephei A]] || {{nobr| 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.
|-
| [[VX Sagittarii]] || 1,350–1,940<ref name="Lockwood">{{cite journal| author1=Lockwood, G.W. |author2=Wing, R. F.| title=The light and spectrum variations of VX Sagittarii, an extremely cool supergiant |journal=[[Monthly Notices of the Royal Astronomical Society]]| volume=198|issue=2| pages=385–404 |year=1982 |bibcode=1982MNRAS.198..385L | doi=10.1093/mnras/198.2.385}}</ref>(–1,520)<ref name=mauron>{{cite journal|bibcode=2011A&A...526A.156M|arxiv=1010.5369|title=The mass-loss rates of red supergiants and the de Jager prescription|journal=Astronomy and Astrophysics|volume=526|pages=A156|author1=Mauron|first1=N.|last2=Josselin|first2=E.|date=2011|doi=10.1051/0004-6361/201013993}}</ref> || VX Sgr is a pulsating variable with a large visual range and varies significantly in size.
|-
| [[SMC 18136]] || 1,310<ref name=mc/> || This would be the largest star in the [[Small Magellanic Cloud|SMC]].
|-
| [[Mu Cephei]] ''([[William Herschel|Herschel]]'s "Garnet Star")'' || 650<ref name=aaa540_2_99>{{Cite journal | first=Takashi | last=Tsuji | title=Water in Emission in the Infrared Space Observatory Spectrum of the Early M Supergiant Star μ Cephei| journal=The Astrophysical Journal Letters | volume=540| issue=2 | pages=99–102 | year=2000 | bibcode=2000ApJ...540L..99T | doi=10.1086/312879|arxiv = astro-ph/0008058 }}</ref>-1,420<ref name=levesqueetal2005/><ref name=josselin>{{cite journal|doi=10.1051/0004-6361:20066353 |title=Atmospheric dynamics and the mass loss process in red supergiant stars |journal=Astronomy and Astrophysics |volume=469 |issue=2 |pages=671–680 |year=2007 |last1=Josselin |first1=E. |last2=Plez |first2=B. |bibcode=2007A&A...469..671J |arxiv = 0705.0266 }}</ref>
|-
| [[BI Cygni]] || 916<ref name=mauron/>-1,240<ref name=levesqueetal2005/>
|-
| [[S Persei]] || 780-1,230<ref name=levesqueetal2005/> || In the Perseus [[ Double Cluster]]
|-
| [[IRC-10414|RAFGL 2139]] ''(IRC-10414)'' || 1,200<ref name="bsp">{{cite journal|bibcode=2014MNRAS.437..843G|title=IRC -10414: A bow-shock-producing red supergiant star|journal=Monthly Notices of the Royal Astronomical Society|volume=437|pages=843|author1=Gvaramadze|first1=V. V.|last2=Menten|first2=K. M.|last3=Kniazev|first3=A. Y.|last4=Langer|first4=N.|last5=MacKey|first5=J.|last6=Kraus|first6=A.|last7=Meyer|first7=D. M.-A.|last8=Kamiński|first8=T.|year=2014|doi=10.1093/mnras/stt1943|arxiv = 1310.2245 }}</ref> || RAFGL 2139 is a red supergiant companion to [[WR 114]].
|-
| [[PZ Cassiopeiae]] || 1,190-1,940<ref name=levesqueetal2005/> || The upper estimate is due to an unusual K band measurement and thought to be an artefact of a reddening correction error. The lower estimate is consistent with other stars in the same survey and with theoretical models.
|-
| [[NML Cygni]] || 1,183<ref name=debeck>{{cite journal|bibcode=2010A&A...523A..18D|arxiv=1008.1083|title=Probing the mass-loss history of AGB and red supergiant stars from CO rotational line profiles. II. CO line survey of evolved stars: Derivation of mass-loss rate formulae|journal=Astronomy and Astrophysics|volume=523|pages=A18|author1=De Beck|first1=E.|last2=Decin|first2=L.|last3=De Koter|first3=A.|last4=Justtanont|first4=K.|last5=Verhoelst|first5=T.|last6=Kemper|first6=F.|last7=Menten|first7=K. M.|year=2010|doi=10.1051/0004-6361/200913771}}</ref>-2,208.5<ref name=zhang/> || NML Cyg is a semiregular variable star surrounded by a circumstellar nebula and is heavily obscured by dust extinction. Previously thought to be as large as {{solar radius|1,650 or 2,775}}.<ref name=zhang>{{Cite journal | last1 = Zhang | first1 = B. | last2 = Reid | first2 = M. J. | last3 = Menten | first3 = K. M. | last4 = Zheng | first4 = X. W. | last5 = Brunthaler | first5 = A. | year = 2012 | title = The distance and size of the red hypergiant NML Cygni from VLBA and VLA astrometry | journal = Astronomy & Astrophysics | volume = 544 | pages = A42 | arxiv = 1207.1850| bibcode = 2012A&A...544A..42Z| doi = 10.1051/0004-6361/201219587 }}</ref>
|-
| [[Betelgeuse]] ''(Alpha Orionis)'' || 1,180<ref name="SMITH2009">{{cite journal |author1=Smith, Nathan |author2=Hinkle, Kenneth H. |author3=Ryde, Nils | title=Red Supergiants as Potential Type IIn Supernova Progenitors: Spatially Resolved 4.6 μm CO Emission Around VY CMa and Betelgeuse | journal=The Astronomical Journal |date=March 2009 | volume=137 | issue=3 | pages=3558–3573 | arxiv=0811.3037 | doi=10.1088/0004-6256/137/3/3558 | bibcode=2009AJ....137.3558S}}</ref><ref name=dolan2016>{{cite journal|doi=10.3847/0004-637X/819/1/7|arxiv=1406.3143v2|title=Evolutionary Tracks for Betelgeuse|journal=The Astrophysical Journal|volume=819|pages=7|year=2016|last1=Dolan|first1=Michelle M.|last2=Mathews|first2=Grant J.|last3=Lam|first3=Doan Duc|last4=Lan|first4=Nguyen Quynh|last5=Herczeg|first5=Gregory J.|last6=Dearborn|first6=David S. P.|bibcode = 2016ApJ...819....7D }}</ref> || Ninth [[List of brightest stars|brightest star]] in the night sky. The angular diameter of Betelgeuse is only exceeded by R Doradus and the Sun.
|-
| [[EV Carinae]] || 1,168<ref name=vanloon>{{cite journal|bibcode=2005A&A...438..273V|arxiv=astro-ph/0504379|title=An empirical formula for the mass-loss rates of dust-enshrouded red supergiants and oxygen-rich Asymptotic Giant Branch stars|journal=Astronomy and Astrophysics|volume=438|pages=273|author1=Van Loon|first1=J. Th.|last2=Cioni|first2=M.-R. L.|last3=Zijlstra|first3=A. A.|last4=Loup|first4=C.|year=2005|doi=10.1051/0004-6361:20042555}}</ref>
|-
| [[BC Cygni]] || 1,140<ref name=levesqueetal2005/> 856–1,553<ref name=turner>{{cite journal|bibcode=2006PASP..118.1533T|title=The Long-Term Behavior of the Semiregular M Supergiant Variable BC Cygni|journal=The Publications of the Astronomical Society of the Pacific|volume=118|issue=849|pages=1533|author1=Turner|first1=David G.|last2=Rohanizadegan|first2=Mina|last3=Berdnikov|first3=Leonid N.|last4=Pastukhova|first4=Elena N.|year=2006|doi=10.1086/508905}}</ref>
|-
| [[RT Carinae]] || 1,090<ref name=levesqueetal2005/>
|-
| [[V396 Centauri]] || 1,070<ref name=levesqueetal2005/>
|-
| [[HV 11423]] || 1,060–1,220<ref name=massey>{{cite journal|bibcode=2007ApJ...660..301M|arxiv=astro-ph/0701769|title=HV 11423: The Coolest Supergiant in the SMC|journal=The Astrophysical Journal|volume=660|pages=301|author1=Massey|first1=Philip|last2=Levesque|first2=Emily M.|last3=Olsen|first3=K. A. G.|last4=Plez|first4=Bertrand|last5=Skiff|first5=B. A.|year=2007|doi=10.1086/513182}}</ref> || HV 11423 is variable in spectral type (observed from K0/1 I to M4.5/5 I), thus probably also in diameter. In October 1978, he appeared as a star of M0I type.
|-
| [[CK Carinae]] || 1,060<ref name=levesqueetal2005/>
|-
| [[V602 Carinae]] || 860<ref name=levesqueetal2005/>-1,050<ref name=torres2015>{{cite journal|bibcode=2015A&A...575A..50A|arxiv=1501.01560|title=What causes the large extensions of red supergiant atmospheres?. Comparisons of interferometric observations with 1D hydrostatic, 3D convection, and 1D pulsating model atmospheres|journal=Astronomy & Astrophysics|volume=575|pages=A50|author1=Arroyo-Torres|first1=B.|last2=Wittkowski|first2=M.|last3=Chiavassa|first3=A.|last4=Scholz|first4=M.|last5=Freytag|first5=B.|last6=Marcaide|first6=J. M.|last7=Hauschildt|first7=P. H.|last8=Wood|first8=P. R.|last9=Abellan|first9=F. J.|year=2015|doi=10.1051/0004-6361/201425212}}</ref>
|-
| [[V1749 Cygni]] || 620-1,040<ref name=levesqueetal2005/>
|-
| [[U Lacertae]] || 384–1,025<ref name=mauron/>
|-
| [[KW Sagittarii]] || 1,009<ref name=torres2013/>-1,460<ref name=levesqueetal2005>Table 4 in {{Cite journal | last1 = Levesque | first1 = E. M. | last2 = Massey | first2 = P. | last3 = Olsen | first3 = K. A. G. | last4 = Plez | first4 = B. | last5 = Josselin | first5 = E. | last6 = Maeder | first6 = A. | last7 = Meynet | first7 = G. | doi = 10.1086/430901 | title = The Effective Temperature Scale of Galactic Red Supergiants: Cool, but Not as Cool as We Thought | journal = The Astrophysical Journal | volume = 628 | issue = 2 | pages = 973 | year = 2005 | pmid = | pmc = |arxiv = astro-ph/0504337 |bibcode = 2005ApJ...628..973L }}</ref> || [[Margin of error|Margin of possible error]]: ± 142 solar radii (Torres 2013).
|-
| [[NR Vulpeculae]] || 980<ref name=levesqueetal2005/>
|-
| [[HV 2112]] || 972<ref name=levesqueetal2014>{{Cite journal|title=Discovery of a Thorne-̇Żytkow object candidate in the Small Magellanic Cloud|journal=Monthly Notices of the Royal Astronomical Society: Letters|volume=443|pages=L94|last=Levesque|first=Emily|author1-link=Emily Levesque|date=1 September 2014|arxiv=1406.0001|bibcode = 2014MNRAS.443L..94L |doi = 10.1093/mnrasl/slu080 }}</ref>
|-
| [[GCIRS 7]] || 960 ± 92<ref name="paumard">{{Cite journal|last1=Paumard |first1=T. |last2=Pfuhl |first2=O. |last3=Martins |first3=F. |last4=Kervella |first4=P. |last5=Ott |first5=T. |last6=Pott |first6=J.-U. |last7=Le Bouquin |first7=J. B. |last8=Breitfelder |first8=J. |last9=Gillessen |first9=S. |last10=Perrin |first10=G. |last11=Burtscher |first11=L. |last12=Haubois |first12=X. |last13=Brandner |first13=W. |title=GCIRS 7, a pulsating M1 supergiant at the Galactic centre. Physical properties and age |journal=Astronomy & Astrophysics |volume=568 |issue=85 |pages=A85 |arxiv=1406.5320 |date=2014 |doi=10.1051/0004-6361/201423991 |bibcode = 2014A&A...568A..85P }}</ref>
|-
| [[S Cassiopeiae]] || 930<ref name=Ramstedt2009>{{cite journal |author1=Ramstedt, S. |author2=Schöier, F. L. |author3=Olofsson, H. | title=Circumstellar molecular line emission from S-type AGB stars: mass-loss rates and SiO abundances | date=2009 | journal=[[Astronomy and Astrophysics]] | volume=499 | number=2 | bibcode=2009A&A...499..515R | doi=10.1051/0004-6361/200911730 | pages=515–527}}</ref><ref name=Ramstedt>{{cite journal | title = Mass-loss properties of S-stars on the AGB | date = 2006 | journal = [[Astronomy and Astrophysics]] | volume = 454 | issue = 2 | pages = L103 | bibcode=2006A&A...454L.103R | author1 = Ramstedt | first1 = S. | last2 = Schöier | first2 = F. L. | last3 = Olofsson | first3 = H. | last4 = Lundgren | first4 = A. A. | doi = 10.1051/0004-6361:20065285 }}</ref> || The largest S-type star existent in [[Milky Way]].{{cn|date=November 2016}}
|-
| [[IX Carinae]] || 920<ref name="levesqueetal2005/>
|-
| [[Antares A]] ''(Alpha Scorpii)'' || 883<ref name=aaa474_1_229>{{cite journal | last1=Baade | first1=R. | last2=Reimers | first2=D. | title=Multi-component absorption lines in the HST spectra of α Scorpii B | journal=Astronomy and Astrophysics | volume=474 | issue=1 | pages=229–237 |date=October 2007 | doi=10.1051/0004-6361:20077308 | bibcode=2007A&A...474..229B }}</ref> (653-1,246<ref group="foot">approximately 800, derived from the 1990 lunar occultation measurement of apparent diameter of 43.1 milliarcsec (up to ±1 milliarcsec error) (http://adsabs.harvard.edu/abs/1990A&A...230..355R page 361) together with 1997 parallax of 5.40 [1.68] milliarcsec ([http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=Antares&submit=SIMBAD+search SIMBAD] citing [http://astrobib.u-strasbg.fr:2008/cgi-bin/cdsbib?1997A%26A...323L..49P Hipparcos]). The parallax gives a derived distance from 460 to 877 light years. This in turn yields an actual diameter from 653 to 1,246 solar radius. An average of 883 is used here.</ref>)
|-
| [[V384 Puppis]] || 500<ref name=mauron/>-850<ref name="levesqueetal2005" />
|-
| [[CW Leonis]] || 826<ref name=debeck />
|-
| [[BO Carinae]] || 790<ref name=levesqueetal2005/>
|-
| [[SU Persei]] || 780<ref name=levesqueetal2005/> || In the Perseus [[ Double Cluster]]
|-
| [[RS Persei]] || 770<ref name="Baron 2014">{{cite journal|bibcode=2014ApJ...785...46B|arxiv = 1405.4032|title = CHARA/MIRC Observations of Two M Supergiants in Perseus OB1: Temperature, Bayesian Modeling, and Compressed Sensing Imaging|journal = The Astrophysical Journal|volume = 785|pages = 46|author1 = Baron|first1 = F.|last2 = Monnier|first2 = J. D.|last3 = Kiss|first3 = L. L.|last4 = Neilson|first4 = H. R.|last5 = Zhao|first5 = M.|last6 = Anderson|first6 = M.|last7 = Aarnio|first7 = A.|last8 = Pedretti|first8 = E.|last9 = Thureau|first9 = N.|last10 = Ten Brummelaar|first10 = T. A.|last11 = Ridgway|first11 = S. T.|last12 = McAlister|first12 = H. A.|last13 = Sturmann|first13 = J.|last14 = Sturmann|first14 = L.|last15 = Turner|first15 = N.|year = 2014|doi = 10.1088/0004-637X/785/1/46}}</ref>-1,000<ref name=levesqueetal2005/> || In the Perseus [[ Double Cluster]]. [[Margin of error|Margin of possible error]]: ± 30 solar radii (Baron 2014).
|-
| [[V355 Cepheus]] || 300<ref name=mauron/>-770<ref name=levesqueetal2005/>
|-
| [[V915 Scorpii]] || 760<ref name=stickland>{{cite journal|bibcode=1985Obs...105..229S|title=IRAS observations of the cool galactic hypergiants|journal=The Observatory|volume=105|pages=229|author1=Stickland|first1=D. J.|year=1985}}</ref>
|-
| [[S Cephei]] || 760<ref name="Bergeat" />
|-
| [[V382 Carinae]] || 747<ref name="achmad">{{cite journal|title=A photometric study of the G0-4 Ia(+) hypergiant HD 96918 (V382 Carinae)|author=Achmad, L.|display-authors=etal|journal=[[Astronomy and Astrophysics]]|volume=259|pages=600–606|year=1992|bibcode=1992A&A...259..600A}}</ref>
|[[Yellow hypergiant]], one of the rarest types of star.
|-
| [[RU Virginis]] || 742<ref name=Bergeat>{{cite journal| author1 = Bergeat, J. |author2= Chevallier, L.| title = The mass loss of C-rich giants| year = 2005| journal = [[Astronomy and Astrophysics]]| volume = 429|pages= 235| number = | id = pp. 235-246| bibcode = 2005A&A...429..235B |doi= 10.1051/0004-6361:20041280}}</ref>
|-
| [[XX Persei]] || 710<ref name=fok>{{cite journal|bibcode=2012ApJ...760...65F|arxiv=1209.6427|title=Maser Observations of Westerlund 1 and Comprehensive Considerations on Maser Properties of Red Supergiants Associated with Massive Clusters|journal=The Astrophysical Journal|volume=760|pages=65|author1=Fok|first1=Thomas K. T.|last2=Nakashima|first2=Jun-Ichi|last3=Yung|first3=Bosco H. K.|last4=Hsia|first4=Chih-Hao|last5=Deguchi|first5=Shuji|year=2012|doi=10.1088/0004-637X/760/1/65}}</ref> (570–1,300{{cn|date=January 2017}}) || In the Perseus [[ Double Cluster]]. The lower size is calculated from mass and luminosity figures. The upper estimate might not be true.
|-
| [[V648 Cassiopeiae]] || 710<ref name="levesqueetal2005" />
|-
| [[TV Geminorum]] || 620-710<ref name=wasatonic>{{cite journal|bibcode=2015PASP..127.1010W|title=V-Band, Near-IR, and TiO Photometry of the Semi-Regular Red Supergiant TV Geminorum: Long-Term Quasi-Periodic Changes in Temperature, Radius, and Luminosity|journal=Publications of the Astronomical Society of Pacific|volume=127|issue=956|pages=1010|author1=Wasatonic|first1=Richard P.|last2=Guinan|first2=Edward F.|last3=Durbin|first3=Allyn J.|year=2015|doi=10.1086/683261}}</ref>(-770<ref name="levesqueetal2005" />)
|-
| [[V528 Carinae]] || 700<ref name="levesqueetal2005" />
|-
| colspan="5" style="text-align:center;"| '''The following well-known stars are listed for the purpose of comparison.'''
|-
| [[RW Cygni]] || 680<ref name=Josselin>{{cite journal| author =| title =Atmospheric dynamics and the mass loss process in red supergiant stars| journal =Astronomy and Astrophysics| year =2007| volume =469| issue =2| pages =671| bibcode = 2007A&A...469..671J| author1 =Josselin| first1 =E.| last2 =Plez| first2 =B.| doi =10.1051/0004-6361:20066353}}</ref>–980<ref name="levesqueetal2005" />
|-
| [[TZ Cassiopeiae]] || 645<ref name=josselin/>–800<ref name="levesqueetal2005" />
|-
| [[Psi1 Aurigae]] || 637{{cn}}
|-
| [[NO Aurigae]] || 630
|-
| [[V1749 Cygni]] || 620-1,040<ref name=levesqueetal2005/> || The upper estimate is due to an unusual [[K band (infrared)|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.
|-
|[[CE Tauri]] ''("Ruby Star")''<ref>[http://jumk.de/astronomie/big-stars/119-tauri.shtml "Big and Giant Stars"]</ref> || 601 ± 83<ref name=vlti>{{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 }}</ref> ||119 Tauri, unofficially nicknamed the Ruby Star. Can be occulted by the Moon, allowing accurate determination of its apparent diameter.
|-
|[[DU Crucis]] || 596<ref name=harris>{{cite journal|bibcode=1976ApJS...30..451H|title=Evolved stars in open clusters|journal=Astrophysical Journal|volume=30|pages=451|author1=Harris|first1=G. L. H.|year=1976|doi=10.1086/190368}}</ref>
|-
| [[S Pegasi]] || 459-574<ref>http://vizier.u-strasbg.fr/viz-bin/VizieR-5?-out.add=.&-source=II/224/cadars&recno=10781</ref>
|-
| [[W Hydrae]] || 562<ref>http://vizier.u-strasbg.fr/viz-bin/VizieR-5?-out.add=.&-source=II/224/cadars&recno=6127</ref>
|-
| [[S Coronae Borealis]] || 537–664<ref name=wallerstein>{{cite journal|bibcode=1977JRASC..71..298W|title=Are long-period variables really pulsating|journal=Journal of the Royal Astronomical Society of Canada|volume=71|pages=298|author1=Wallerstein|first1=G.|year=1977}}</ref>
|-
| [[R Andromedae]] || 485 ± 125
|-
| [[Chi Cygni]] || 348–480<ref>http://vizier.u-strasbg.fr/viz-bin/VizieR-5?-out.add=.&-source=II/224/cadars&recno=9107</ref>
|-
| [[R Hydrae]] || 460
|-
|[[Rho Cassiopeiae]] || 450 ± 50<ref name=gorlova>{{Cite journal | last1 = Gorlova | first1 = N. | last2 = Lobel | first2 = A. | last3 = Burgasser | first3 = A. J. | last4 = Rieke | first4 = G. H. | last5 = Ilyin | first5 = I. | last6 = Stauffer | first6 = J. R. | doi = 10.1086/507590 | title = On the CO Near‐Infrared Band and the Line‐splitting Phenomenon in the Yellow Hypergiant ρ Cassiopeiae | journal = The Astrophysical Journal | volume = 651 | issue = 2 | pages = 1130–1150 | year = 2006 | pmid = | pmc = |arxiv = astro-ph/0607158 |bibcode = 2006ApJ...651.1130G }}</ref> || [[Yellow hypergiant]], one of the rarest types of a star.
|-
| [[Eta Carinae A]] ''(Tseen She)'' || 430 ± 370<ref name=gull>{{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 | year = 2010 |arxiv = 0910.3158 |bibcode = 2010HiA....15..373G }}</ref> || Previously thought to be the most massive single star, but in 2005 it was realized to be a binary system. Its size is poorly defined.
|-
| [[S Orionis]] || 411–498<ref name=wittkowski>{{cite journal|bibcode=2007A&A...470..191W|arxiv=0705.4614|title=The Mira variable S Orionis: Relationships between the photosphere, molecular layer, dust shell, and SiO maser shell at 4 epochs|journal=Astronomy and Astrophysics|volume=470|pages=191|author1=Wittkowski|first1=M.|last2=Boboltz|first2=D. A.|last3=Ohnaka|first3=K.|last4=Driebe|first4=T.|last5=Scholz|first5=M.|year=2007|doi=10.1051/0004-6361:20077168}}</ref>
|-
|[[R Leporis]] || 400 ± 90<ref name=hofmann>{{cite journal|bibcode=2005ESASP.560..651H|title=Interferometric observations of the Mira star o Ceti with the VLTI/VINCI instrument in the near-infrared|journal=Proceedings of the 13th Cambridge Workshop on Cool Stars|volume=560|pages=651|author1=Hofmann|first1=K.-H.|last2=Eberhardt|first2=M.|last3=Driebe|first3=T.|last4=Schertl|first4=D.|last5=Scholz|first5=M.|last6=Schoeller|first6=M.|last7=Weigelt|first7=G.|last8=Wittkowski|first8=M.|last9=Woodruff|first9=H. C.|year=2005}}</ref> || One of the largest carbon stars existent in the [[Milky Way]].
|-
| [[V509 Cassiopeiae]] || 400<ref>http://vizier.u-strasbg.fr/viz-bin/VizieR-5?-out.add=.&-source=II/224/cadars&recno=10628</ref>–900<ref name="Nugent">{{cite web |first=Richard |last=Nugent |publisher=weblore.com |url=http://www.weblore.com/richard/garnet_star.htm |title=The Garnet Star |quote=DIAM .. m Cep 1224 ... V509 CAS 910 ... V382 CAR 747 |accessdate=2009-12-04}}</ref>
|-
| [[La Superba]] ''(Y Canum Venaticorum)'' || 390<ref name=luttermoser>{{cite journal|bibcode=1992ApJ...384..634L|title=A VLA 3.6 centimeter survey of N-type carbon stars|journal=Astrophysical Journal|volume=384|pages=634|author1=Luttermoser|first1=Donald G.|last2=Brown|first2=Alexander|year=1992|doi=10.1086/170905}}</ref>|| Currently one of the coolest and reddest stars.
|-
| [[V838 Monocerotis]] || 380 ± 90<ref name=tylenda>{{Cite journal | last1 = Tylenda | first1 = R. | last2 = Kamiński | first2 = T. | last3 = Schmidt | first3 = M. | last4 = Kurtev | first4 = R. | last5 = Tomov | first5 = T. | title = High-resolution optical spectroscopy of V838 Monocerotis in 2009 | doi = 10.1051/0004-6361/201116858 | journal = Astronomy & Astrophysics | volume = 532 | pages = A138 | date = 2011 |arxiv = 1103.1763 |bibcode = 2011A&A...532A.138T }}</ref> || V838 Mon is a new type of object known as a [[Luminous red nova]]. The very large cool "{{C|L-type supergiants|L-type supergiant}}" reported with this large radius is a transient object which will contract rapidly over a few decades. Once topped to the list as one of the largest stars. Lane ''et al'' originally estimated the radius of V838 Mon to be at 1,570 ± 400 solar radii.
|-
| [[S Doradus]] || 100–380<ref name="lamers1995">{{cite conference | last=Lamers | first=H. J. G. L. M. | contribution=Observations and Interpretation of Luminous Blue Variables | title=Proceedings of IAU Colloquium 155, Astrophysical applications of stellar pulsation | journal=Astrophysical applications of stellar pulsation. Astronomical Society of the Pacific Conference Series | volume=83 | pages=176–191 | date=February 6–10, 1995 | location=Cape Town, South Africa | publisher=Astronomical Society of the Pacific | bibcode=1995ASPC...83..176L }}</ref> || Prototype [[Luminous Blue Variable|S Doradus variable]].
|-
| [[U Orionis]] || 370 ± 96
|-
| [[R Doradus]] || 370 ± 50<ref name=mnras286_4_957>{{citation | display-authors=1 | last1=Bedding | first1=T. R. | author1-link = Tim Bedding | last2=Zijlstra | first2=A. A. | last3=von der Luhe | first3=O. | last4=Robertson | first4=J. G. | last5=Marson | first5=R. G. | last6=Barton | first6=J. R. | last7=Carter | first7=B. S. | title=The angular diameter of R Doradus: a nearby Mira-like star | journal=Monthly Notices of the Royal Astronomical Society | volume=286 | issue=4 | pages=957–962 | date=April 1997 | bibcode=1997MNRAS.286..957B | arxiv=astro-ph/9701021 | doi=10.1093/mnras/286.4.957}}</ref> || Star with the second largest apparent size after the Sun.
|-
| [[R Leonis]] || 320–350<ref>{{cite journal |arxiv=astro-ph/0411133 |author1=Fedele |author2=Wittkowski |author3=Paresce |author4=Scholz |author5=Wood |author6=Ciroi |doi=10.1051/0004-6361:20042013 |title=The K-band intensity profile of R Leonis probed by VLTI/VINCI |year=2004 |bibcode=2005A&A...431.1019F |journal=Astronomy and Astrophysics |volume=431 |issue=3 |pages=1019–1026}}</ref>
|-
| [[V337 Carinae]] || 350
|-
|[[The Pistol Star]] || 346 ± 40<ref name=najarro>{{Cite journal | last1 = Najarro | first1 = F. | last2 = Figer | first2 = D. F. | last3 = Hillier | first3 = D. J. | last4 = Geballe | first4 = T. R. | last5 = Kudritzki | first5 = R. P. | title = Metallicity in the Galactic Center: The Quintuplet Cluster | doi = 10.1088/0004-637X/691/2/1816 | journal = The Astrophysical Journal | volume = 691 | issue = 2 | pages = 1816 | year = 2009 | pmid = | pmc = |arxiv = 0809.3185 |bibcode = 2009ApJ...691.1816N }}</ref> || Blue [[hypergiant]], currently among the [[List of most massive stars|most massive]] and [[List of most luminous stars|luminous stars]].
|-
| [[Mira A]] ''(Omicron Ceti)'' || 332–402<ref name=aaa421>{{cite journal | last=Woodruff | first=H. C. |last2=Eberhardt |first2=M. | last3=Driebe | first3=T. | last4=Hofmann | first4=K.-H. | last5=Ohnaka | first5=K. | last6=Richichi | first6=A. | last7=Schert | first7=D. | last8=Schöller | first8=M. | last9=Scholz | first9=M. | last10=Weigelt | first10=G. | last11=Wittkowski | first11=M. | last12=Wood | first12=P. R. |display-authors=4| title=Interferometric observations of the Mira star o Ceti with the VLTI/VINCI instrument in the near-infrared | journal=Astronomy & Astrophysics | date=2004 | volume=421 | issue=2 | pages=703–714 | doi=10.1051/0004-6361:20035826 | bibcode=2004A&A...421..703W |arxiv = astro-ph/0404248 }}</ref> || Prototype [[Mira variable]].
|-
| [[T Cephei]] || 329<ref name=gerd>{{cite journal|author=Gerd Weigelt et al.|journal=SPIE|bibcode=2003SPIE.4838..181W|title=JHK-band spectro-interferometry of T Cep with the IOTA interferometer|volume=4838|pages=181|pp=181–184|date=2003|doi=10.1117/12.458659|series=Interferometry for Optical Astronomy II}}</ref>
|-
| [[V381 Cephei]] || 327
|-
| [[Pi Puppis]] || 290
|-
|[[Alpha Herculis]] A ''(Ras Algethi)'' || 264–303<ref name=moravveji>{{cite journal|bibcode=2013AJ....146..148M|arxiv=1308.1632|title=The Age and Mass of the α Herculis Triple-star System from a MESA Grid of Rotating Stars with 1.3 <= M/M ⊙ <= 8.0|journal=The Astronomical Journal|volume=146|issue=6|pages=148|author1=Moravveji|first1=Ehsan|last2=Guinan|first2=Edward F.|last3=Khosroshahi|first3=Habib|last4=Wasatonic|first4=Rick|year=2013|doi=10.1088/0004-6256/146/6/148}}</ref>
|-
| [[R Cassiopeiae]] || 263<ref name=takeuti>{{cite journal|bibcode=2013PASJ...65...60T|title=A Method to Estimate the Masses of Asymptotic Giant Branch Variable Stars|journal=Publications of the Astronomical Society of Japan|volume=65|issue=3|pages=60|author1=Takeuti|first1=Mine|last2=Nakagawa|first2=Akiharu|last3=Kurayama|first3=Tomoharu|last4=Honma|first4=Mareki|year=2013|doi=10.1093/pasj/65.3.60}}</ref>
|-
| [[Cygnus OB2-12]] || 246
|-
| [[Delta Canis Majoris]] ''(Wezen)'' || 237 ± 66<ref>{{cite journal|last= Davis J, Booth AJ, Ireland MJ, Jacob AP, North JR, Owens SM, Robertson JG, Tango WJ, Tuthill PG|year=2007|first1= J.|pages= 151|last2= Booth|first2= A. J.|last3= Ireland|first3= M. J.|last4= Jacob|first4= A. P.|last5= North|first5= J. R.|issue= 3|last6= Owens|first6= S. M.|last7= Robertson|first7= J. G.|last8= Tango|first8= W. J.|last9= Tuthill|first9= P. G.|volume= 24|title=The Emergent Flux and Effective Temperature of Delta Canis Majoris|journal= Publications of the Astronomical Society of Australia|doi=10.1071/AS07017|arxiv=0709.3873|bibcode = 2007PASA...24..151D }}</ref> || 36th [[List of brightest stars|brightest star]] in the night sky.
|-
| [[LBV 1806-20]] || 150–236
|-
| [[Zeta Cephei]] || 230<ref name=wesselink>{{cite journal|bibcode=1972A&AS....7..257W|title=Catalogue of stellar dimensions|journal=Astronomy and Astrophysics Supplement|volume=7|pages=257|author1=Wesselink|first1=A. J.|last2=Paranya|first2=K.|last3=Devorkin|first3=K.|year=1972}}</ref>
|-
| [[HR Carinae]] || 220<ref name=boffin>{{cite journal|bibcode=2016A&A...593A..90B|title=The LBV HR Car has a partner: Discovery of a companion with the VLTI |arxiv=1607.07724|author1=Boffin|first1=Henri M. J.|last2=Rivinius|first2=Thomas|last3=Merand|first3=Antoine|last4=Mehner|first4=Andrea|last5=Lebouquin|first5=Jean-Baptiste|last6=Pourbaix|first6=Dimitri|last7=De Wit|first7=Willem-Jan|last8=Martayan|first8=Christophe|last9=Guieu|first9=Sylvain|year=2016|doi=10.1051/0004-6361/201629127|journal=Astronomy & Astrophysics|volume=593 |pages=A90 }}</ref>
|-
| [[Deneb]] A ''(Alpha Cygni)''|| 220 ± 17<ref name=schiller>
{{cite journal |last1=Schiller |first1=F. |last2=Przybilla |first2=N. |date=2008 |title=Quantitative spectroscopy of Deneb |journal=[[Astronomy & Astrophysics]] |volume=479 |issue=3 |pages=849–858 |arxiv=0712.0040 |bibcode=2008A&A...479..849S |doi=10.1051/0004-6361:20078590}}</ref> || 19th [[List of brightest stars|brightest star]] in the night sky.
|-
| [[Omicron¹ Canis Majoris|Omicron<sup>1</sup> Canis Majoris]] || 231
|-
| [[V810 Centauri]] || 210
|-
| [[Zeta Aurigae]] ''(Haedus)'' || 200<ref>http://www.hposoft.com/EAur09/ZetaAurigae.html</ref>
|-
| [[Delta² Lyrae|Delta<sup>2</sup> Lyrae]] || 200
|-
| [[Lambda Velorum]] ''(Al Suhail)''|| 200
|-
| [[RS Puppis]] || 200
|-
| [[Epsilon Pegasi]] ''(Enif)'' || 185
|-
| [[L Carinae]] || 179
|-
| [[6 Cassiopeiae]] || 170
|-
| [[Rho Persei]] ''(Gorgonea Tertia)''|| 164
|-
| [[Epsilon Carinae]] ''(Avior)''|| 153
|-
| [[Gamma Cygni]] ''(Sadir)'' || 150
|-
| [[Epsilon Geminorum]] ''(Mebsuta)'' || 150
|-
| [[V533 Carinae]] ''(VV Storm)'' || 141.5<ref name=snow>{{cite journal|bibcode=1994ApJS...95..163S|title=An atlas of ultraviolet P Cygni profiles|journal=The Astrophysical Journal Supplement Series|volume=95|pages=163|author1=Snow|first1=Theodore P.|last2=Lamers|first2=Henny J. G. L. M.|last3=Lindholm|first3=Douglas M.|last4=Odell|first4=Andrew P.|year=1994|doi=10.1086/192099}}</ref>
|-
| [[Epsilon Aurigae]] A ''(Almaaz)'' || 135–190 || Epsilon Aurigae was incorrectly hailed as the largest known star before 1970 with a radius around {{solar radius|2,700–3,000}} ({{solar radius|295-2,600}} for Epsilon Aurigae B), even though it later turned out not to be an ''infrared light star'' but rather a dusk torus surrounding the system.
|-
| [[Mu Boötis]] ''(Alkalurops)''|| 130
|-
| [[66 Andromedae]] || 130
|-
| [[QS Aquilae]] || 130
|-
| [[56 Aquilae]] || 130
|-
| [[HD 56096|L Puppis]] || 126
|-
| [[Iota¹ Scorpii|Iota Scorpii]] ''(Apollyon)''|| 125
|-
| [[Delta Apodis]] || 125
|-
| [[HIP 110307]] || 124.1
|-
| [[32 G. Hydrae]] || 121.7
|-
| [[HD 84810|I Carinae]] || 120
|-
| [[Xi Puppis]] ''(Asmidiske)'' || 120
|-
| [[Mu Sagittarii]] ''(Polis)''|| 115
|-
| [[Omicron2 Cygni|Omicron Cygni]] || 115
|-
| [[Gamma Aquilae]] ''(Tarazed)'' || 110
|-
| [[34 Boötis]] || 110
|-
| [[Beta Arae]] || 110
|-
| [[Alpha Trianguli Australis|Atria]] (Alpha Trianguli Australis) || 109
|-
| [[Beta Cygni]] A1 ''(Albireo)'' || 109<ref name=jumk>{{cite web |title=Albireo |url=https://jumk.de/astronomie/big-stars/albireo.shtml|date= |work=Big and Giant Stars |publisher= |accessdate=}}</ref>
|-
| [[Beta Pegasi]] ''(Scheat)''|| 95
|-
| [[WR 102ka|Peony Nebula Star]] || 92<ref name="barniske">{{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 | pmid = | pmc = |arxiv = 0807.2476 |bibcode = 2008A&A...486..971B }}</ref> || Candidate for most luminous star in the Milky Way.
|-
| [[17 Camelopardalis]] || 91.3
|-
| [[Beta Andromedae]] ''(Mirach)'' || 90
|-
| [[R Scuti]] || 87.4
|-
| [[Gamma Crucis]] ''(Gacrux)'' || 84<ref name=snow>{{cite journal|bibcode=1994ApJS...95..163S|title=An atlas of ultraviolet P Cygni profiles|journal=The Astrophysical Journal Supplement Series|volume=95|pages=163|author1=Snow|first1=Theodore P.|last2=Lamers|first2=Henny J. G. L. M.|last3=Lindholm|first3=Douglas M.|last4=Odell|first4=Andrew P.|year=1994|doi=10.1086/192099}}</ref>
|-
| [[Nu Cephei]] || 83.5
|-
| [[Gamma Andromedae]] ''(Almach)''|| 83
|-
| [[Theta Herculis]] ''(Rukbalgethi Genubi)''|| 80
|-
| [[Var 83]] || 80
|-
| [[Rigel A]] ''(Beta Orionis A)'' || 78.9 ± 7.4<ref name=apj2012_747_108>{{cite journal | last1=Moravveji | first1=Ehsan | last2=Guinan | first2=Edward F. | last3=Shultz | first3=Matt | last4=Williamson | first4=Michael H. | last5=Moya | first5=Andres | title=Asteroseismology of the nearby SN-II Progenitor: Rigel. Part I. The ''MOST'' High-precision Photometry and Radial Velocity Monitoring | journal=The Astrophysical Journal | volume=747 | issue=1 | pages=108–115 |date=March 2012 | doi=10.1088/0004-637X/747/2/108 | bibcode=2012ApJ...747..108M |arxiv = 1201.0843 }}</ref> || Seventh [[List of brightest stars|brightest star]] in the night sky.
|-
| [[Alpha Leporis]] ''(Arneb)'' || 77
|-
| [[P Cygni]] || 76
|-
| [[Beta Doradus]] || 76
|-
| [[DL Crucis]] || 75-80
|-
| [[Pi Herculis]] || 72
|-
| [[Canopus]] ''(Alpha Carinae)'' || 71 ± 7<ref name=vlti/> || Second [[List of brightest stars|brightest star]] in the night sky.
|-
| [[13 Boötis]] || 71
|-
| [[62 Sagittarii]] || 70
|-
| [[Nu Aquilae]] ''(Equator Star)''|| 66
|-
| [[R Coronae Borealis]] || 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
|-
| [[Chi² Orionis|Chi Orionis]] || 59
|-
| [[Alpha Persei]] ''(Mirfak)'' || 56
|-
| [[Iota Aurigae]] ''(Al Kab)'' || 55
|-
| [[FF Aquilae]] || 55
|-
| [[Alpha Apodis]] || 55
|-
| [[Tau¹ Serpentis|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|HD 5980 A]] || 48-160
|-
| [[Epsilon Boötis]] ''(Izar)'' || 48
|-
| [[Zeta² Scorpii]] || 48
|-
| [[AG Antliae]] || 47
|-
| [[HD 3346|V428 Andromedae]] || 46.3
|-
| [[HD 13189]] || 46
|-
| [[HD 203857]] || 46
|-
|[[Aldebaran]] A ''(Alpha Tauri)'' || 44.2 ± 0.9<ref name=richichi>{{cite journal|author1=Richichi, A.|author2=Roccatagliata, V.|title=Aldebaran's angular diameter: how well do we know it?|date=2005|doi=10.1051/0004-6361:20041765|journal=Astronomy and Astrophysics|volume=433|pages=305–312|arxiv=astro-ph/0502181|bibcode=2005A&A...433..305R}}</ref>
|-
| [[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|HD 5980 B]] || 40
|-
| [[Eta Canis Majoris]] ''(Aludra)'' || 37.8
|-
| [[Polaris]] ''(Alpha Ursae Minoris)'' || 37.5<ref name=fadeyev>{{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|pages=1011|year=2015|last1=Fadeyev|first1=Y. A.}}</ref> ||The current northern [[pole star]].
|-
| [[87 Leonis]] || 37
|-
| [[Gamma Centauri]] ''(Muhlifan)'' || 36.5
|-
| [[S Normae]] || 35.6
|-
|[[R136a1]] || 35.4<ref name="arxiv">{{Cite journal |last1=Crowther |first1=P. A. |last2=Schnurr |first2=O. |last3=Hirschi |first3=R. |last4=Yusof |first4=N. |last5=Parker |first5=R. J. |last6=Goodwin |first6=S. P. |last7=Kassim |first7=H. A. |year=2010 |title=The R136 star cluster hosts several stars whose individual masses greatly exceed the accepted 150 M<sub>⊙</sub> stellar mass limit |journal=[[Monthly Notices of the Royal Astronomical Society]] |volume=408 |issue=2 |pages=731 |arxiv=1007.3284 |bibcode=2010MNRAS.408..731C |doi=10.1111/j.1365-2966.2010.17167.x }}</ref> || Also on the list as the most massive and luminous star.
|-
| [[Sher 25]] || 35
|-
| [[Gamma Leonis]] ''(Algieba)'' || 31.9
|-
| [[Alpha Camelopardalis]] || 31.2
|-
| [[Alpha Ursae Majoris]] ''(Dubhe)'' || 30
|-
| [[11 Lacertae]] || 30
|-
| [[Beta Camelopardalis]] || 30
|-
| [[Cyg OB2 -8A|Cygnus OB2-8]] || 28
|-
| [[Eta Leonis]] ''(Al Jabhah)''|| 27
|-
| [[QPM-241]] ''(Archen Star)'' || 27
|-
| [[R Apodis]] || 26.3
|-
| [[Epsilon Orionis]] ''(Alnilam)'' || 26
|-
| [[Eta Piscium]] ''(Kullat Nunu)''|| 26
|-
| [[Melnick 42]] || 26
|-
| [[Arcturus]] ''(Alpha Boötis)'' || 25.4<ref name=ramirez_prieto_2011>{{Cite journal|bibcode=2011ApJ...743..135R|title=Fundamental Parameters and Chemical Composition of Arcturus|journal=[[The Astrophysical Journal]]|volume=743|issue=2|pages=135|date=December 2011 |author=I. Ramírez|author2=C. Allende Prieto|doi=10.1088/0004-637X/743/2/135|arxiv = 1109.4425 }}</ref>|| Brightest star in the northern hemisphere
|-
| [[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
|-
|[[HDE 226868]] || 20–22<ref name=MNRAS358_3_851>{{citation | last=Ziółkowski | first=J. | title=Evolutionary constraints on the masses of the components of HDE 226868/Cyg 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}} Note: for radius and luminosity, see Table 1 with ''d''=2 kpc.</ref> || The supergiant companion of black hole Cygnus X-1. The black hole is 500,000 times smaller than the star (or 58.4388 km in diameter).
|-
| [[Zeta Orionis]] ''(Alnitak)'' || 20
|-
| [[Theta Scorpii]] ''(Sargas)'' || 20
|-
| [[Beta Herculis]] ''(Kornephoros)'' || 20
|-
| [[Theta Apodis]] || 20
|-
| [[Alpha Sagittae]] ''(Alsahm)''|| 20
|-
| Stars of [[Westerlund 2]] || 19.3
|-
| [[Plaskett's star|HR 2422 Monocerotis]] ''(Plaskett's Star)'' || 19.2
|-
| [[Kappa Cassiopeiae]] || 19
|-
| [[Beta Scorpii]] ''(Acrab)'' || 19
|-
| [[Beta Lyrae]] ''(Sheliak)'' || 19
|-
| [[Zeta Puppis]] ''(Naos)'' || 18.6
|-
| [[HD 269810|R 122]] || 18.5
|-
| [[HD 93250]] || 18
|-
| [[Alpha Microscopii]] || 17.5
|-
| [[LH54-425|LH45-425 A]] || 17.5
|-
| [[Upsilon1 Hydrae|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
|-
| [[VV Cephei B]] || 13<ref name=wright1977>{{cite journal|bibcode=1977JRASC..71..152W|title=The system of VV Cephei derived from an analysis of the H-alpha line|journal=Journal of the Royal Astronomical Society of Canada|volume=71|pages=152|author1=Wright|first1=K. O.|year=1977}}</ref>–25<ref name=hack>{{cite journal|bibcode=1992A&AS...95..589H|title=Spectroscopic study of the atmospheric eclipsing binary VV Cephei|journal=Astronomy and Astrophysics Supplement Series (ISSN0365-0138)|volume=95|pages=589|author1=Hack|first1=M.|last2=Engin|first2=S.|last3=Yilmaz|first3=N.|last4=Sedmak|first4=G.|last5=Rusconi|first5=L.|last6=Boehm|first6=C.|year=1992}}</ref> || The B-type main sequence companion of [[VV Cephei A]].
|-
| [[37 Aquilae]] || 13
|-
| [[HD 240210]] || 13
|-
| [[Capella (star)|Alpha Aurigae A]] ''(Capella A)'' || 12.2
|-
| [[Xi Aquilae]] || 12
|-
| [[Gamma Arae]] || 12
|-
| [[Gamma Sagittarii]] ''(Alnasl)'' || 11
|-
| [[WR 104]] || 10 ||In 389,400 years, this [[Wolf-Rayet star]] is expected to explode in a supernova. It has been suggested that it may produce a gamma ray burst that could pose a threat to life on Earth should its poles be aligned 12° or lower towards Earth. This will probably cause the [[Holocene extinction|Holocene exinction event]]. The star's axis of rotation has yet to be determined with certainty.
|-
| [[LH54-425|LH45-425 B]] || 10
|-style="background:pink;" class="sortbottom"
|[[Sun]] || 1<ref name=IAU2015resB3>{{citation | first1=E.E. | last1=Mamajek | first2=A. | last2=Prsa | first3=G. | last3=Torres | first4=al. | last4=et | title=IAU 2015 Resolution B3 on Recommended Nominal Conversion Constants for Selected Solar and Planetary Properties | arxiv=1510.07674}}</ref> || The largest object in the [[solar system]]. <br><small>The core hydrogen would be exhausted in 5.4 billion years. In 7.647 billion years, The Sun would reach the tip of the red-giant branch of the [[Hertzsprung–Russell diagram]], achieving its size of {{solar radius|256 to 436|link=y}}.<ref name="Rybicki2001" > {{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><ref name="Schroder 2008" > {{cite journal | last1 = Schroder | first1 = K. P. | last2 = Connon Smith | first2 = Robert | date = 2008 | title = Distant Future of the Sun and Earth Revisited | journal = Monthly Notices of the Royal Astronomical Society | volume = 386 | issue = 1 | pages = 155–163 | bibcode = 2008MNRAS.386..155S | doi = 10.1111/j.1365-2966.2008.13022.x |arxiv = 0801.4031 }} </ref></small><br/> <small> Reported for reference </small>
|}
== Timeline of largest star recordholders ==
{{Disputed-section|Timeline|date=August 2016}}
{|class=wikitable
|-
! Star
! Size ({{solar radius}})
! Date
!class="unsortable"| Notes
|-
| {{nowrap|[[UY Scuti]]}}
| 1,708 ± 192<ref name="torres2013" />
| Nov 2015—
| [[Margin of error]] in size determination: ± 192 solar radii. At its smallest, its size would be similar to that of [[V354 Cephei]]. At its largest, its size would be 1,900 solar radii.
|-
| [[NML Cygni]]
| 2,208.5 ± 566.5
| June 2015–Nov 2015
|-
| {{nowrap|[[UY Scuti]]}}
| 1,708 ± 192<ref name="torres2013" />
| Oct 2013—Nov 2015
| [[Margin of error]] in size determination: ± 192 solar radii. At its smallest, its size would be similar to that of [[V354 Cephei]]. At its largest, its size would be 1,900 solar radii.
|-
| {{nowrap|[[Westerlund 1-26]]}}
| 1,951–2,544<ref>{{cite journal|doi=10.1051/0004-6361/201116990|title=A VLT/FLAMES survey for massive binaries in Westerlund 1|journal=Astronomy & Astrophysics|volume=531|pages=A28|year=2011|last1=Clark|first1=J. S.|last2=Ritchie|first2=B. W.|last3=Negueruela|first3=I.|last4=Crowther|first4=P. A.|last5=Damineli|first5=A.|last6=Jablonski|first6=F. J.|last7=Langer|first7=N.|bibcode=2011A&A...531A..28C}}</ref><ref>{{Cite journal|arxiv=1209.6427v1|author1=Fok|author2=Jun-ichi Nakashima|author3=Yung|author4=Chih-Hao Hsia|author5=Shuji Deguchi|title=Maser Observations of Westerlund 1 and Comprehensive Considerations on Maser Properties of Red Supergiants Associated with Massive Clusters|journal=The Astrophysical Journal|volume=760|pages=65|year=2012|doi=10.1088/0004-637X/760/1/65|bibcode=2012ApJ...760...65F}}</ref><ref>{{cite journal|doi=10.1051/0004-6361/200913820|title=A serendipitous survey for variability amongst the massive stellar population of Westerlund 1|journal=Astronomy and Astrophysics|volume=514|pages=A87|year=2010|last1=Clark|first1=J. S.|last2=Ritchie|first2=B. W.|last3=Negueruela|first3=I.|bibcode=2010A&A...514A..87C}}</ref>
| Sept 2012—Oct 2013
| Very uncertain parameters for an unusual star with strong radio emission. The spectrum is variable but apparently the luminosity is not.
|-
| [[KY Cygni]]
| 2,850<ref name="levesqueetal2005" />
| August 2012–Sept 2012
|
|-
| [[WOH G64]]
| 1,730–2,474
| July 2012–August 2012
|
|-
| {{nowrap|[[NML Cygni]]}}
| 1,650–2,775<ref>{{cite journal|doi=10.1051/0004-6361/201219587|title=The distance and size of the red hypergiant NML Cygni from VLBA and VLA astrometry|journal=Astronomy & Astrophysics|volume=544|pages=A42|year=2012|last1=Zhang|first1=B.|last2=Reid|first2=M. J.|last3=Menten|first3=K. M.|last4=Zheng|first4=X. W.|last5=Brunthaler|first5=A.|bibcode=2012A&A...544A..42Z}}</ref>
| 2012—July 2012
| NML Cyg is a semiregular variable star surrounded by a circumstellar nebula and is heavily obscured by dust extinction.
|-
| {{nowrap|[[VY Canis Majoris]]}}
| 1,950 (1,800–2,100)
| 2007—2012
| Previously thought to be a star so large that it contradicted stellar evolutionary theory, a newly improved measurement has brought it down to size.
|-
| {{nowrap|[[VV Cephei A]]}}
| 1,750 ({{nowrap|1,600<ref>{{cite journal |author=Habets, G. M. H. J.; Heintze, J. R. W. |title=Empirical bolometric corrections for the main-sequence |journal=Astronomy and Astrophysics Supplement |volume=46 | date=November 1981 |pages=193–237 |bibcode=1981A&AS...46..193H}} Page 225 "Table IV" #178</ref>–1,900<ref name="Kaler">
{{cite web |title=VV CEP (VV Cephei)|publisher=University of Illinois|author=Professor James B. (Jim) Kaler|url=http://www.astro.uiuc.edu/~kaler/sow/vvcep.html|accessdate=2010-03-15
}}</ref><ref name="levesqueetal2005" />}}) (possibly 2,640)
| 2006—2007
| VV Cep A is a highly distorted star in a binary system, losing mass to its B-type companion VV Cephei B for at least part of its orbit.
|-
| {{nowrap|[[Mu Cephei]]}}
| 1,800 (1,650–2,536<ref name=levesqueetal2005/>)
| June 2005–2006
|
|-
| [[KY Cygni]]
| 2,850<ref name="levesqueetal2005" />
| 2005–June 2005
|
|-
| [[V838 Monocerotis]]
| 1,970<ref name="Lane2005">{{cite journal | last = Lane | first = B. F. | last2 = Retter | first2 = A. | last3 = Thompson | first3 = R. R. | last4 = Eisner | first4 = J. A. | title = Interferometric Observations of V838 Monocerotis | journal = The Astrophysical Journal | volume = 622 | issue = 2 | pages = L137–L140 | publisher = The American Astronomical Society | date = April 2005 | arxiv = astro-ph/0502293 | doi = 10.1086/429619 | bibcode=2005ApJ...622L.137L}}</ref>
| 2002–2005
|
|-
| {{nowrap|[[EV Carinae]]}}
| 2,880<ref name=dejager>{{cite journal|bibcode=1988A&AS...72..259D|title=Mass loss rates in the Hertzsprung-Russell diagram|journal=Astronomy and Astrophysics|volume=72|pages=259-289|author1=de Jager|first1=C.|last2=Nieuwenhuijzen|first2=H.|last3=van der Hucht|first3=K.A.|year=1988}}</ref>
| 2 Feb 1988–2002
|
|-
| {{nowrap|[[VX Sagittarii]]}}
| 1,940<ref name="Lockwood" />
| 1982—2 Feb 1988
|
|-
| {{nowrap|[[VV Cephei A]]}}
| {{nowrap|1,600<ref>{{cite journal |author=Habets, G. M. H. J.; Heintze, J. R. W. |title=Empirical bolometric corrections for the main-sequence |journal=Astronomy and Astrophysics Supplement |volume=46 | date=November 1981 |pages=193–237 |bibcode=1981A&AS...46..193H}} Page 225 "Table IV" #178</ref>–1,900<ref name="Kaler">
{{cite web |title=VV CEP (VV Cephei)|publisher=University of Illinois|author=Professor James B. (Jim) Kaler|url=http://www.astro.uiuc.edu/~kaler/sow/vvcep.html|accessdate=2010-03-15
}}</ref><ref name="levesqueetal2005" />}}
| 1970—1982
| VV Cep A is a highly distorted star in a binary system, losing mass to its B-type companion VV Cephei B for at least part of its orbit.
|-
| {{nowrap|[[Epsilon Aurigae]]}}
| 2,700-3,000
|........—1970|| Epsilon Aurigae was incorrectly hailed as the largest known star before 1970, even though it later turned out not to be an 'infrared light star' but rather a dusk torus surrounding the system.
|}
== Relations between Solar radius and Orbital radius of planets ==
{| class="wikitable"
|+'''List of orbital radius of planets '''
|-
! style="background-color:#EFEFEF;white-space: nobr;" | Planet
! style="background-color:#deadff;white-space: nobr;" | [[Astronomical unit]]<br/> (AU = 1.49597870691 × 10<sup>8</sup>km = 214.9 solar radii)
! style="background-color:#ffdead;white-space: nobr;width:11em" | [[Solar radius|Solar radii]]<br/> ([[Sun]] = 695,742 km)
! style="background-color:#EFEFEF;white-space: nobr;" | Example stars
|-
||[[Mercury]] || 0.31 - 0.47 || 66 - 100 || [[Canopus]] (71) [[Rigel]] (78.9) [[Beta Cygni]] (109)
|-
||[[Venus]] || 0.72 - 0.73 || 154 - 157 || [[Epsilon Pegasi]] (185)
|-
||[[Earth]] || 0.98 - 1.02 || 211 - 219 || [[Deneb]] (220) [[LBV 1806-20]] (150–236) [[Alpha Herculis]] (264–303)
|-
||[[Mars]] || 1.38 - 1.67 || 297 - 358 || [[Mira]] (332-402) [[Pistol Star]] (346) [[Chi Cygni]] (348-480) [[Epsilon Aurigae]] (143-358) [[V838 Monocerotis]] (380) [[La Superba]] (390)
|-
||Inner limits of the [[Asteroid Belt]] || 1.92 || 412 || [[Eta Carinae]] (430) [[Rho Cassiopeiae]] (450) [[S Pegasi]] (580) [[V1749 Cygni]] (620-1,040) [[TZ Cassiopeiae]] (645) [[RW Cygni]] (680-980) [[TV Geminorum]] (620-710) [[V382 Carinae]] (747) [[S Persei]] (780-1,230)
|-
||Outer limits of the [[Asteroid Belt]] || 3.79 || 816 || [[CW Leonis]] (826) [[Antares]] (883) [[KW Sagittarii]] (1,009-1,460)
|-
||[[Jupiter]] || 4.95 - 5.46 || 1,064 - 1,173 || [[EV Carinae]] (1,168) [[Betelgeuse]] (887–1,180) [[NML Cygni]] (1,183) [[Mu Cephei]] (1,260) [[VV Cephei]] (1,050-1,900) [[VY Canis Majoris]] (1,420) [[KY Cygni]] (1,420-2,850) [[HR 5171]] (<!--1,315--->1,490) [[WOH G64]] (1,540-1,730) [[V838 Monocerotis]] (Lane ''et al'' estimate) (1,570) [[NML Cygni]] (Zhang ''et al'' estimate) (1,650) [[UY Scuti]] (1,708)
|-
||[[Saturn]] || 9.02 - 10.08 || 1,940 - 2,169 || None - some obsolete historical estimates are given for context: [[VY Canis Majoris]] (Humphreys ''et al'' estimate) (1,800-2,252) [[Westerlund 1-26]] (Clark ''et al'' estimate) (1,951–2,544) Star size limit (2,600) [[NML Cygni]] (upper estimate) (2,775) [[KY Cygni]] (upper estimate) (2,850) [[EV Carinae]] (upper estimate) (2,880)<!-- [[UY Scuti]] (Possible upper estimate) (3,000)-->
|-
||[[Uranus]] ||18.33 - 20.11 || 3,941 - 4,324 ||
|-
||[[Neptune]] ||29.81 - 30.33 || 6,411 - 6,526 ||
|-
||[[Pluto]] ||29.658 - 49.305 || 6,377 - 10,602 ||
|-
||[[Planet Nine]] (Also known as ''Phattie'')||200 - 1,200|| 43,006 - 258,039 ||
|}
==See also==
{{Portal|Star}}
{{cmn|colwidth=30em|
* [[Constellation]]
* [[Lists of stars]]
* [[List of most massive stars]]
* [[List of most luminous stars]]
* [[List of hottest stars]]
* [[List of coolest stars]]
* [[List of most massive black holes]]
* [[List of largest nebulae]]
* [[List of largest galaxies]]
* [[List of largest cosmic structures]]
* [[List of largest exoplanets]]
* [[List of star extremes]]
}}
==References==
{{reflist|30em}}
==External links==
* [http://www.giant-stars.de/ Giant Stars] An interactive website comparing the Earth and the Sun to some of the largest stars
* [http://news.bbc.co.uk/2/hi/science/nature/4164365.stm BBC News] Three largest stars identified
* [http://www.universetoday.com/2008/04/06/what-is-the-biggest-star-in-the-universe/ Universe Today] What is the Biggest Star in the Universe?
{{Top 10 largest stars}}
{{Star}}
This is a list of [[star]]s which are the least voluminous known (the smallest stars by volume).
==List==
{{expand list|date=January 2015}}
===Notable small stars===
{| class="wikitable sortable"
|-
! Star !! Star mean radius, km !! Star class !!Refs!!Notes
|-
|| [[A.C.+70°8247]] || 1.048656438 ||[[white dwarf]]||<ref>{{cite journal |title= The White Dwarf A.C.+70°8247, the Smallest Star Known |author= Kuiper, G. P. |date= February 1936 |journal= Journal of the Royal Astronomical Society of Canada |volume= 30 |page= 48 |bibcode= 1936JRASC..30...48K }}</ref>||Smallest white dwarf star known
|-
|| [[XTE J1650-500]] B || 24 ||[[black hole]]||<ref>{{cite journal |title= The White Dwarf A.C.+70°8247, the Smallest Star Known |author= Kuiper, G. P. |date= February 1936 |journal= Journal of the Royal Astronomical Society of Canada |volume= 30 |page= 48 |bibcode= 1936JRASC..30...48K }}</ref>||This binary X-ray transient system, XTE J1650-500, component black hole, at 3.8 solar masses, is smaller than the previous recordholder GRO J1655-40 B of 6.3 MSun in the microquasar system GRO J1655-40.
|-
|| [[Sirius B]] || 5,466 ||[[white dwarf]]||<ref>[https://www.jstor.org/stable/40678784?seq=1#page_scan_tab_contents Temperature, radius, and rotational velocity of sirius b]</ref>||Historically first detected white dwarf star
|-
|| [[Beta Cygni|Beta Cygni Ab]] (unconfirmed) || 6,000 ||[[brown dwarf]]|| ||Smallest brown dwarf known
|-
|| [[Procyon B]] || 8,584.938 ||[[white dwarf]]||<ref>name="Levesque2009"</ref><ref>[http://iopscience.iop.org/article/10.1086/304003/fulltext/35322.text.html Wide Field Planetary Camera 2 Photometry of the Bright, Mysterious White Dwarf Procyon B]</ref>||
|-
|| [[40 Eridani B]] || 9,739.8 || [[white dwarf]]||<ref name="hippmr">{{cite journal|bibcode=1998ApJ...494..759P|title=Testing the White Dwarf Mass-Radius Relation with HIPPARCOS|journal=The Astrophysical Journal|volume=494|issue=2|pages=759|author1=Provencal|first1=J. L.|last2=Shipman|first2=H. L.|last3=Høg|first3=Erik|last4=Thejll|first4=P.|year=1998|doi=10.1086/305238}}</ref>||
|-
|| [[2MASS J0523-1403]] || 60,000 ||[[red dwarf]]||<ref name=SnT-2013-12-23>{{cite news |url= http://www.skyandtelescope.com/astronomy-news/new-cutoff-for-star-sizes/ |title= New Cutoff for Star Sizes |author= John Bochanski |date= 23 December 2013 |publisher= Sky and Telescope }}</ref><ref name=2014AJ....147...94D/>||This red dwarf is considered (as in 2013) the smallest star known, and representative of the smallest star possible, which is not a [[brown dwarf]] or a [[degenerate dwarf|dead star]].
|-
|| [[SSSPM J0829-1309]] || 61,300 ||[[red dwarf]]||<ref name=2014AJ....147...94D>{{cite journal |author1=Sergio B. Dieterich |author2=Todd J. Henry |author3=Wei-Chun Jao |author4=Jennifer G. Winters |author5=Altonio D. Hosey |author6=Adric R. Riedel |author7=John P. Subasavage |title= The Solar Neighborhood XXXII. The Hydrogen Burning Limit |journal= The Astronomical Journal |volume= 147 |issue= 5 |id= 94 |page= 25 |date= May 2014 |doi= 10.1088/0004-6256/147/5/94 |bibcode= 2014AJ....147...94D |arxiv= 1312.1736 }}</ref>||
|-
|| [[TRAPPIST-1]] || 79,400 ||[[red dwarf]]||<ref name="Gillon2017">{{cite journal|url=http://www.eso.org/public/archives/releases/sciencepapers/eso1706/eso1706a.pdf |title=Seven temperate terrestrial planets around the nearby ultracool dwarf star TRAPPIST-1|journal= Nature|volume= 542|issue= 7642|pages= 456|doi= 10.1038/nature21360|year= 2017|last1= Gillon|first1=M.|last2= Triaud|first2=A. H. M. J.|last3= Demory|first3=B.-O.|last4= Jehin|first4= E.|last5= Agol|first5=E.|last6= Deck|first6=K. M.|last7= Lederer|first7=S. M.|last8=De Wit|first8=J.|last9= Burdanov|first9=A.|last10= Ingalls|first10=J. G.|last11= Bolmont|first11=E.|last12= Leconte|first12=J.|last13= Raymond|first13=S. N.|last14= Selsis|first14=F.|last15= Turbet|first15=M.|last16= Barkaoui|first16=K.|last17= Burgasser|first17=A.|last18= Burleigh|first18=M. R.|last19= Carey|first19=S. J.|last20= Chaushev|first20=A.|last21= Copperwheat|first21=C. M.|last22= Delrez|first22=L.|last23= Fernandes|first23=C. S.|last24= Holdsworth|first24=D. L.|last25= Kotze|first25=E. J.|last26= Van Grootel|first26=V.|last27= Almleaky|first27=Y.|last28= Benkhaldoun|first28=Z.|last29= Magain|first29=P.|last30= Queloz|first30=D.}}</ref>||Hosts a planetary system with at least seven rocky planets
|-
|| [[OGLE-TR-122B]] || 81,100 ||[[red dwarf]]||<ref name=Space-2005-03-03>{{cite news |url= http://www.space.com/840-newfound-star-smaller-planets.html |title= Newfound Star Smaller than Some Planets |author= Robert Roy Britt |date= 3 March 2005 |publisher= Space.com }}</ref><ref name=SpaceAnswers-SmallestStar-2013-03-22>{{cite web |url= http://www.spaceanswers.com/deep-space/what-is-the-smallest-star/ |title= What is the smallest star? |author1= Jonathan O'Callaghan |author2= Josh Barker (National Space Centre) |date= 22 March 2013 |publisher= SpaceAnswers.com }}</ref><ref name=2005A&A...433L..21P>{{cite journal |title= A planet-sized transiting star around OGLE-TR-122. Accurate mass and radius near the hydrogen-burning limit |arxiv= astro-ph/0501611 |doi= 10.1051/0004-6361:200500025 |bibcode= 2005A&A...433L..21P |author1=Pont, F. |author2=Melo, C. H. F. |author3=Bouchy, F. |author4=Udry, S. |author5=Queloz, D. |author6=Mayor, M. |author7=Santos, N. C. |publicationdate= April 2005 |journal= Astronomy and Astrophysics |volume= 433 |issue= 2 |page= L21-L24 |date= 27 January 2005 }}</ref><ref name=Space-2005-03-03/><ref name=SpaceAnswers-SmallestStar-2013-03-22/><ref name=2005A&A...433L..21P/>||This was once the smallest known actively fusing star, when found in 2005, through 2013. It is the smallest eclipsing red dwarf, and smallest observationally measured diameter.
|-
|| [[Proxima Centauri]] || 98,093.7 ||[[red dwarf]]||<ref name=2009A&A...505..205D>{{cite journal |title= Mass-radius relation of low and very low-mass stars revisited with the VLTI |bibcode= 2009A&A...505..205D |doi= 10.1051/0004-6361/200911976 |arxiv= 0906.0602 |author1=B.-O. Demory |author2=D. Segransan |author3=T. Forveille |author4=D. Queloz |author5=J.-L. Beuzit |author6=X. Delfosse |author7=E. Di Folco |author8=P. Kervella |author9=J.-B. Le Bouquin |author10=C. Perrier |journal= Astronomy and Astrophysics |volume= 505 |issue= 1 |pages= 205–215 |publicationdate= October 2009 |date= 2 June 2009 }}</ref>||This is the nearest neighbouring star to the Sun.
|-
|}
This is a list of [[star]]s which are the least voluminous known (the smallest stars by volume).
==List==
{{expand list|date=January 2015}}
{| class="wikitable sortable"
|-
! style="background:#efefef; white-space:nobr;"| {{nowrap|Star name}}
! style="background:#ffdead; white-space:nobr;"| Radius<br/>{{nowrap|[[Estimated Jupiter radius|Solar radii]]}}<br/><small>{{nowrap|1=([[Jupiter]] = 1)}}</small>
! style="background:#deadff; white-space:nobr;"| Radius<br/>{{nowrap|[[Estimated Sun radius|Jupiter radii]]}}<br/><small>{{nowrap|1=([[Sun]] = 1)}}</small>
!width=100%| Notes
!|
|-
|| [[Sirius B]] || 0.7733333333 || 0.0828571428 ||
|-
|| [[Procyon B]] || 0.8733333333 || 0.00935714285 || <ref>name="Levesque2009"</ref>
|-
|| [[Teegarden's Star]] || 0 || 0 ||
|-
|| [[2MASS J0523-1403]] || 0 || 0 ||
|-
|| [[The Sun]] || 1 || 1000 ||
|}
== Smallest by type ==
{| class="wikitable sortable"
|+'''List of the smallest stars by star type'''
|-
! style="background:#000000; color:#ffffff; white-space:nobr;"| Type
! style="background:#efefef; white-space:nobr;"| {{nowrap|Star name}}
! style="background:#ffdead; white-space:nobr;"| Radius<br/>{{nowrap|[[Solar radius|Solar radii]]}}<br/><small>{{nowrap|1=([[Sun]] = 1)}}</small>
! style="background:#deadff; white-space:nobr;"| Radius<br/>{{nowrap|[[Jupiter radius|Jupiter radii]]}}<br/><small>{{nowrap|1=([[Jupiter]] = 1)}}</small>
! style="background:#deffad; white-space:nobr;"| Radius<br/>{{nowrap|[[Earth radius|Earth radii]]}}<br/><small>{{nowrap|1=([[Earth]] = 1)}}</small>
! style="background:#c0c0c0; white-space:nobr;"| Radius<br/><small>{{nowrap|([[kilometre|km]] / [[statute mile|mi]])}}</small>
!| Date
!width=100%| Notes
!|
|-
|| [[Red dwarf]]
|| [[2MASS J0523-1403]]
|| 0.086
|| .896
|| 9.39
||
|| 2013
|| This red dwarf is considered the smallest star known, and representative of the smallest star possible, which is not a [[brown dwarf]] or a [[degenerate dwarf|dead star]].
|| <ref name=SnT-2013-12-23>{{cite news |url= http://www.skyandtelescope.com/astronomy-news/new-cutoff-for-star-sizes/ |title= New Cutoff for Star Sizes |author= John Bochanski |date= 23 December 2013 |publisher= Sky and Telescope }}</ref>
|-
|| [[Brown dwarf]]
||
||
||
||
||
||
||
||
|-
|| [[White dwarf]]
|| [[A.C.+70°8247]]
|| 0.00000150734
|| 0.00157316804
|| 0.5
||
|| 1934
||
|| <ref>{{cite journal |title= The White Dwarf A.C.+70°8247, the Smallest Star Known |author= Kuiper, G. P. |date= February 1936 |journal= Journal of the Royal Astronomical Society of Canada |volume= 30 |page= 48 |bibcode= 1936JRASC..30...48K }}</ref>
|-
|| [[Neutron star]]
||
||
||
||
||
||
||
||
|-
|| [[Stellar-mass black hole]]
|| [[XTE J1650-500 B]]
||
||
||
|| {{convert|24|km|mi|abbr=on}}
|| 2008
|| This binary X-ray transient system, [[XTE J1650-500]], component black hole, at 3.8 [[solar mass]]es, is smaller than the previous recordholder [[GRO J1655-40 B]] of 6.3 M<sub>Sun</sub> in the microquasar system [[GRO J1655-40]].
|| <ref name=Space-2008-04-01>{{cite news |url= http://www.space.com/5191-smallest-black-hole.html |title= Smallest Black Hole Found |author= Andrea Thompson |date= 1 April 2008 |publisher= Space.com }}</ref>
|-
|}
==Smallest active stars==
This is a listing of the smallest stars that are incontrovertibly stars that are still alive and fusing. Hence they are the smallest [[red dwarf]]s known, and those [[brown dwarf]]s that are known to be still in their short actively fusing phase.
{| class="wikitable sortable"
|+'''List of the smallest live stars'''
|-
! style="background:#efefef; white-space:nobr;"| {{nowrap|Star name}}
! style="background:#ffdead; white-space:nobr;"| Radius<br>{{nowrap|[[Solar radius|Solar radii]]}}<br><small>{{nowrap|1=([[Sun]] = 1)}}</small>
! style="background:#deadff; white-space:nobr;"| Radius<br>{{nowrap|[[Jupiter radius|Jupiter radii]]}}<br><small>{{nowrap|1=([[Jupiter]] = 1)}}</small>
!| Type
!width=100%| Notes
!|
|-
|| [[SSSPM J0829-1309]]
|| 0.088
|| .917
|| Red dwarf
||
|| <ref name=2014AJ....147...94D>{{cite journal |author1=Sergio B. Dieterich |author2=Todd J. Henry |author3=Wei-Chun Jao |author4=Jennifer G. Winters |author5=Altonio D. Hosey |author6=Adric R. Riedel |author7=John P. Subasavage |title= The Solar Neighborhood XXXII. The Hydrogen Burning Limit |journal= The Astronomical Journal |volume= 147 |issue= 5 |id= 94 |page= 25 |date= May 2014 |doi= 10.1088/0004-6256/147/5/94 |bibcode= 2014AJ....147...94D |arxiv= 1312.1736 }}</ref>
|-
|| [[OGLE-TR-122B]]
|| 0.120
|| 1.16
|| Red dwarf
|| This was once the smallest known actively fusing star, when found in 2005, through 2013. It is the smallest eclipsing red dwarf, and smallest observationally measured diameter.
|| <ref name=Space-2005-03-03>{{cite news |url= http://www.space.com/840-newfound-star-smaller-planets.html |title= Newfound Star Smaller than Some Planets |author= Robert Roy Britt |date= 3 March 2005 |publisher= Space.com }}</ref><ref name=SpaceAnswers-SmallestStar-2013-03-22>{{cite web |url= http://www.spaceanswers.com/deep-space/what-is-the-smallest-star/ |title= What is the smallest star? |author1= Jonathan O'Callaghan |author2= Josh Barker (National Space Centre) |date= 22 March 2013 |publisher= SpaceAnswers.com }}</ref><ref name=2005A&A...433L..21P>{{cite journal |title= A planet-sized transiting star around OGLE-TR-122. Accurate mass and radius near the hydrogen-burning limit |arxiv= astro-ph/0501611 |doi= 10.1051/0004-6361:200500025 |bibcode= 2005A&A...433L..21P |author1=Pont, F. |author2=Melo, C. H. F. |author3=Bouchy, F. |author4=Udry, S. |author5=Queloz, D. |author6=Mayor, M. |author7=Santos, N. C. |publicationdate= April 2005 |journal= Astronomy and Astrophysics |volume= 433 |issue= 2 |page= L21-L24 |date= 27 January 2005 }}</ref>
|-
|| [[Proxima Centauri]]
|| 0.145
|| 1.510
|| Red dwarf
|| This is the nearest neighbouring star to the Sun.
|| <ref name=2005A&A...433L..21P/><ref name=2009A&A...505..205D>{{cite journal |title= Mass-radius relation of low and very low-mass stars revisited with the VLTI |bibcode= 2009A&A...505..205D |doi= 10.1051/0004-6361/200911976 |arxiv= 0906.0602 |author1=B.-O. Demory |author2=D. Segransan |author3=T. Forveille |author4=D. Queloz |author5=J.-L. Beuzit |author6=X. Delfosse |author7=E. Di Folco |author8=P. Kervella |author9=J.-B. Le Bouquin |author10=C. Perrier |journal= Astronomy and Astrophysics |volume= 505 |issue= 1 |pages= 205–215 |publicationdate= October 2009 |date= 2 June 2009 }}</ref>
|-
|| [[Barnard's Star]]
|| 0.196
|| 2.042
|| Red dwarf
||
|| <ref name=2005A&A...433L..21P/><ref name=2009A&A...505..205D/>
|-
|| [[CM Draconis B]]
|| 0.2396
|| 2.496
|| Red dwarf
|| Part of the binary red dwarf system [[CM Draconis]]
|| <ref name=2005A&A...433L..21P/><ref name=2009ApJ...691.1400M>{{cite journal |title= Absolute properties of the low-mass eclipsing binary CM Draconis |author1=J.C. Morales |author2=I. Ribas |author3=C. Jordi |author4=G. Torres |author5=J. Gallardo |author6=E.F. Guinan |author7=D. Charbonneau |author8=M. Wolf |author9=D.W. Latham |author10=G. Anglada-Escudé |author11=D.H. Bradstreet |author12=M.E. Everett |author13=F.T. O'Donovan |author14=G. Mandushev |author15=R.D. Mathieu |arxiv= 0810.1541 |bibcode= 2009ApJ...691.1400M |doi= 10.1088/0004-637X/691/2/1400 |publicationdate= February 2009 |orig-year= 8 October 2008 |journal= The Astrophysical Journal |volume= 691 |issue= 2 |pages= 1400–1411 }}</ref>
|-
|| [[CM Draconis A]]
|| 0.2534
|| 2.640
|| Red dwarf
|| Part of the binary red dwarf system [[CM Draconis]]
|| <ref name=2005A&A...433L..21P/><ref name=2009ApJ...691.1400M/>
|-
|| [[Kapteyn's Star]]
|| 0.291
|| 3.031
|| Red dwarf
|| This is the closest halo star to the Sun.
|| <ref name=2005A&A...433L..21P/><ref name=2009A&A...505..205D/>
|-
|}
{| class="wikitable sortable"
|+'''Timeline of smallest live star recordholders'''
|-
! style="background:#efefef; white-space:nobr;"| {{nowrap|Star name}}
!| Date
! style="background:#ffdead; white-space:nobr;"| Radius<br>{{nowrap|[[Solar radius|Solar radii]]}}<br><small>{{nowrap|1=([[Sun]] = 1)}}</small>
! style="background:#deadff; white-space:nobr;"| Radius<br>{{nowrap|[[Jupiter radius|Jupiter radii]]}}<br><small>{{nowrap|1=([[Jupiter]] = 1)}}</small>
!| Type
!width=100%| Notes
!|
|-
|| [[2MASS J0523-1403]]
|| 2013—
|| 0.086
|| .896
|| [[Red dwarf]]
|| This [[red dwarf]] is considered the smallest star known, and representative of the smallest star possible that is not a [[brown dwarf]].
|| <ref name=SnT-2013-12-23/><ref name=2014AJ....147...94D/>
|-
|| [[OGLE-TR-122B]]
|| 2005-2013
|| 0.120
|| 1.16
|| Red dwarf
|| This is the smallest eclipsing red dwarf, and smallest observationally measured diameter.
|| <ref name=Space-2005-03-03/><ref name=SpaceAnswers-SmallestStar-2013-03-22/><ref name=2005A&A...433L..21P/>
|-
|}
==List==
{{expand list|date=January 2015}}
{| class="wikitable sortable"
|-
! style="background:#efefef; white-space:nobr;"| {{nowrap|Star name}}
! style="background:#ffdead; white-space:nobr;"| Radius<br/>{{nowrap|[[Estimated Jupiter radius|Solar radii]]}}<br/><small>{{nowrap|1=([[Jupiter]] = 1)}}</small>
! style="background:#deadff; white-space:nobr;"| Radius<br/>{{nowrap|[[Estimated Sun radius|Jupiter radii]]}}<br/><small>{{nowrap|1=([[Sun]] = 1)}}</small>
!width=100%| Notes
!|
|-
|| [[Sirius B]] || 0.7733333333 || 0.0828571428 ||
|-
|| [[Procyon B]] || 0.8733333333 || 0.00935714285 || <ref>name="Levesque2009"</ref>
|-
|| [[Teegarden's Star]] || 0 || 0 ||
|-
|| [[2MASS J0523-1403]] || 0 || 0 ||
|-
|| [[The Sun]] || 1 || 1000 ||
|}
== Smallest by type ==
{| class="wikitable sortable"
|+'''List of the smallest stars by star type'''
|-
! style="background:#000000; color:#ffffff; white-space:nobr;"| Type
! style="background:#efefef; white-space:nobr;"| {{nowrap|Star name}}
! style="background:#ffdead; white-space:nobr;"| Radius<br/>{{nowrap|[[Solar radius|Solar radii]]}}<br/><small>{{nowrap|1=([[Sun]] = 1)}}</small>
! style="background:#deadff; white-space:nobr;"| Radius<br/>{{nowrap|[[Jupiter radius|Jupiter radii]]}}<br/><small>{{nowrap|1=([[Jupiter]] = 1)}}</small>
! style="background:#deffad; white-space:nobr;"| Radius<br/>{{nowrap|[[Earth radius|Earth radii]]}}<br/><small>{{nowrap|1=([[Earth]] = 1)}}</small>
! style="background:#c0c0c0; white-space:nobr;"| Radius<br/><small>{{nowrap|([[kilometre|km]] / [[statute mile|mi]])}}</small>
!| Date
!width=100%| Notes
!|
|-
|| [[Red dwarf]]
|| [[2MASS J0523-1403]]
|| 0.086
|| .896
|| 9.39
||
|| 2013
|| This red dwarf is considered the smallest star known, and representative of the smallest star possible, which is not a [[brown dwarf]] or a [[degenerate dwarf|dead star]].
|| <ref name=SnT-2013-12-23>{{cite news |url= http://www.skyandtelescope.com/astronomy-news/new-cutoff-for-star-sizes/ |title= New Cutoff for Star Sizes |author= John Bochanski |date= 23 December 2013 |publisher= Sky and Telescope }}</ref>
|-
|| [[Brown dwarf]]
||
||
||
||
||
||
||
||
|-
|| [[White dwarf]]
|| [[A.C.+70°8247]]
|| 0.00000150734
|| 0.00157316804
|| 0.5
||
|| 1934
||
|| <ref>{{cite journal |title= The White Dwarf A.C.+70°8247, the Smallest Star Known |author= Kuiper, G. P. |date= February 1936 |journal= Journal of the Royal Astronomical Society of Canada |volume= 30 |page= 48 |bibcode= 1936JRASC..30...48K }}</ref>
|-
|| [[Neutron star]]
||
||
||
||
||
||
||
||
|-
|| [[Stellar-mass black hole]]
|| [[XTE J1650-500 B]]
||
||
||
|| {{convert|24|km|mi|abbr=on}}
|| 2008
|| This binary X-ray transient system, [[XTE J1650-500]], component black hole, at 3.8 [[solar mass]]es, is smaller than the previous recordholder [[GRO J1655-40 B]] of 6.3 M<sub>Sun</sub> in the microquasar system [[GRO J1655-40]].
|| <ref name=Space-2008-04-01>{{cite news |url= http://www.space.com/5191-smallest-black-hole.html |title= Smallest Black Hole Found |author= Andrea Thompson |date= 1 April 2008 |publisher= Space.com }}</ref>
|-
|}
==Smallest active stars==
This is a listing of the smallest stars that are incontrovertibly stars that are still alive and fusing. Hence they are the smallest [[red dwarf]]s known, and those [[brown dwarf]]s that are known to be still in their short actively fusing phase.
{| class="wikitable sortable"
|+'''List of the smallest live stars'''
|-
! style="background:#efefef; white-space:nobr;"| {{nowrap|Star name}}
! style="background:#ffdead; white-space:nobr;"| Radius<br>{{nowrap|[[Solar radius|Solar radii]]}}<br><small>{{nowrap|1=([[Sun]] = 1)}}</small>
! style="background:#deadff; white-space:nobr;"| Radius<br>{{nowrap|[[Jupiter radius|Jupiter radii]]}}<br><small>{{nowrap|1=([[Jupiter]] = 1)}}</small>
!| Type
!width=100%| Notes
!|
|-
|| [[SSSPM J0829-1309]]
|| 0.088
|| .917
|| Red dwarf
||
|| <ref name=2014AJ....147...94D>{{cite journal |author1=Sergio B. Dieterich |author2=Todd J. Henry |author3=Wei-Chun Jao |author4=Jennifer G. Winters |author5=Altonio D. Hosey |author6=Adric R. Riedel |author7=John P. Subasavage |title= The Solar Neighborhood XXXII. The Hydrogen Burning Limit |journal= The Astronomical Journal |volume= 147 |issue= 5 |id= 94 |page= 25 |date= May 2014 |doi= 10.1088/0004-6256/147/5/94 |bibcode= 2014AJ....147...94D |arxiv= 1312.1736 }}</ref>
|-
|| [[OGLE-TR-122B]]
|| 0.120
|| 1.16
|| Red dwarf
|| This was once the smallest known actively fusing star, when found in 2005, through 2013. It is the smallest eclipsing red dwarf, and smallest observationally measured diameter.
|| <ref name=Space-2005-03-03>{{cite news |url= http://www.space.com/840-newfound-star-smaller-planets.html |title= Newfound Star Smaller than Some Planets |author= Robert Roy Britt |date= 3 March 2005 |publisher= Space.com }}</ref><ref name=SpaceAnswers-SmallestStar-2013-03-22>{{cite web |url= http://www.spaceanswers.com/deep-space/what-is-the-smallest-star/ |title= What is the smallest star? |author1= Jonathan O'Callaghan |author2= Josh Barker (National Space Centre) |date= 22 March 2013 |publisher= SpaceAnswers.com }}</ref><ref name=2005A&A...433L..21P>{{cite journal |title= A planet-sized transiting star around OGLE-TR-122. Accurate mass and radius near the hydrogen-burning limit |arxiv= astro-ph/0501611 |doi= 10.1051/0004-6361:200500025 |bibcode= 2005A&A...433L..21P |author1=Pont, F. |author2=Melo, C. H. F. |author3=Bouchy, F. |author4=Udry, S. |author5=Queloz, D. |author6=Mayor, M. |author7=Santos, N. C. |publicationdate= April 2005 |journal= Astronomy and Astrophysics |volume= 433 |issue= 2 |page= L21-L24 |date= 27 January 2005 }}</ref>
|-
|| [[Proxima Centauri]]
|| 0.145
|| 1.510
|| Red dwarf
|| This is the nearest neighbouring star to the Sun.
|| <ref name=2005A&A...433L..21P/><ref name=2009A&A...505..205D>{{cite journal |title= Mass-radius relation of low and very low-mass stars revisited with the VLTI |bibcode= 2009A&A...505..205D |doi= 10.1051/0004-6361/200911976 |arxiv= 0906.0602 |author1=B.-O. Demory |author2=D. Segransan |author3=T. Forveille |author4=D. Queloz |author5=J.-L. Beuzit |author6=X. Delfosse |author7=E. Di Folco |author8=P. Kervella |author9=J.-B. Le Bouquin |author10=C. Perrier |journal= Astronomy and Astrophysics |volume= 505 |issue= 1 |pages= 205–215 |publicationdate= October 2009 |date= 2 June 2009 }}</ref>
|-
|| [[Barnard's Star]]
|| 0.196
|| 2.042
|| Red dwarf
||
|| <ref name=2005A&A...433L..21P/><ref name=2009A&A...505..205D/>
|-
|| [[CM Draconis B]]
|| 0.2396
|| 2.496
|| Red dwarf
|| Part of the binary red dwarf system [[CM Draconis]]
|| <ref name=2005A&A...433L..21P/><ref name=2009ApJ...691.1400M>{{cite journal |title= Absolute properties of the low-mass eclipsing binary CM Draconis |author1=J.C. Morales |author2=I. Ribas |author3=C. Jordi |author4=G. Torres |author5=J. Gallardo |author6=E.F. Guinan |author7=D. Charbonneau |author8=M. Wolf |author9=D.W. Latham |author10=G. Anglada-Escudé |author11=D.H. Bradstreet |author12=M.E. Everett |author13=F.T. O'Donovan |author14=G. Mandushev |author15=R.D. Mathieu |arxiv= 0810.1541 |bibcode= 2009ApJ...691.1400M |doi= 10.1088/0004-637X/691/2/1400 |publicationdate= February 2009 |orig-year= 8 October 2008 |journal= The Astrophysical Journal |volume= 691 |issue= 2 |pages= 1400–1411 }}</ref>
|-
|| [[CM Draconis A]]
|| 0.2534
|| 2.640
|| Red dwarf
|| Part of the binary red dwarf system [[CM Draconis]]
|| <ref name=2005A&A...433L..21P/><ref name=2009ApJ...691.1400M/>
|-
|| [[Kapteyn's Star]]
|| 0.291
|| 3.031
|| Red dwarf
|| This is the closest halo star to the Sun.
|| <ref name=2005A&A...433L..21P/><ref name=2009A&A...505..205D/>
|-
|}
{| class="wikitable sortable"
|+'''Timeline of smallest live star recordholders'''
|-
! style="background:#efefef; white-space:nobr;"| {{nowrap|Star name}}
!| Date
! style="background:#ffdead; white-space:nobr;"| Radius<br>{{nowrap|[[Solar radius|Solar radii]]}}<br><small>{{nowrap|1=([[Sun]] = 1)}}</small>
! style="background:#deadff; white-space:nobr;"| Radius<br>{{nowrap|[[Jupiter radius|Jupiter radii]]}}<br><small>{{nowrap|1=([[Jupiter]] = 1)}}</small>
!| Type
!width=100%| Notes
!|
|-
|| [[2MASS J0523-1403]]
|| 2013—
|| 0.086
|| .896
|| [[Red dwarf]]
|| This [[red dwarf]] is considered the smallest star known, and representative of the smallest star possible that is not a [[brown dwarf]].
|| <ref name=SnT-2013-12-23/><ref name=2014AJ....147...94D/>
|-
|| [[OGLE-TR-122B]]
|| 2005-2013
|| 0.120
|| 1.16
|| Red dwarf
|| This is the smallest eclipsing red dwarf, and smallest observationally measured diameter.
|| <ref name=Space-2005-03-03/><ref name=SpaceAnswers-SmallestStar-2013-03-22/><ref name=2005A&A...433L..21P/>
|-
|}
== References ==
{{reflist}}
{{star}}
This is a '''list of coolest stars''' discovered, arranged by decreasing temperature. The stars with [[temperature]]s lower than 3,000 [[Kelvin|K]] are included.
==List==
{{Expand list|date=October 2016}}
{| class="wikitable sortable"
|-
! Star name
! Temperature<br>([[Kelvin|K]])
! Notes
|-
|[[WISE J0855-0714]]
|225–260<ref name="NASA20140425">{{cite news |url=http://www.nasa.gov/jpl/wise/spitzer-coldest-brown-dwarf-20140425/ |title=NASA's Spitzer and WISE Telescopes Find Close, Cold Neighbor of Sun |work=[[NASA]].gov |first1=Whitney |last1=Clavin |first2=J. D. |last2=Harrington |date=25 April 2014 |archiveurl=https://web.archive.org/web/20140426004939/http://www.nasa.gov/jpl/wise/spitzer-coldest-brown-dwarf-20140425 |archivedate=26 April 2014 |deadurl=no}}</ref>
|
|-
|[[CFBDSIR 1458+10B]]
|370
|
|-
|[[2MASS 0939-2448]] A/B
|650<ref name="Leggett2009">{{cite journal |last1=Leggett |first1=S. K. |last2=Cushing |first2=Michael C. |last3=Saumon |first3=D. |last4=Marley |first4=M. S. |last5=Roellig |first5=T. L. |last6=Warren |first6=S. J. |last7=Burningham |first7=Ben |last8=Jones |first8=H. R. A. |last9=Kirkpatrick |first9=J. D. |last10=Lodieu |first10=N. |last11=Lucas |first11=P. W. |last12=Mainzer |first12=A. K. |last13=Martín |first13=E. L. |last14=McCaughrean |first14=M. J. |last15=Pinfield |first15=D. J. |last16=Sloan |first16=G. C. |last17=Smart |first17=R. L. |last18=Tamura |first18=M. |last19=Van Cleve |first19=J. |title=The Physical Properties of Four ~600 K T Dwarfs |date=2009 |journal=[[The Astrophysical Journal]] |volume=695| issue=2 | pages=1517–1526 |arxiv=0901.4093 |doi=10.1088/0004-637X/695/2/1517 |bibcode=2009ApJ...695.1517L}}</ref>
|
|-
|[[2MASS 0415-0935]]
|764
|
|-
|[[2M 1237+6526]]
| 850<ref name="Liebert & Burgasser">{{cite journal | arxiv=astro-ph/0609793| author=Liebert| author2=Burgasser| last-author-amp=yes| title=On the Nature of the Unique Hα-emitting T Dwarf 2MASS J12373919+6526148| journal=[[Astronomy & Astrophysics]]| volume=655|issue=1|pages=522–527 |date=2007|bibcode=2007ApJ...655..522L|doi = 10.1086/509882 }}</ref>
|
|-
|[[SCR 1845-6357B]]
|950
|
|-
|[[2MASS 0243-2453]]
|1,050
|
|-
|[[Cha 110913-773444]]
|1,350
|
|-
|[[2MASS 0036+1821]]
|1,650
|
|-
|[[2MASS 1507-1627]]
|1,650
|
|-
|[[OTS 44]]
|1,700
|
|-
|[[S Cassiopeiae]]
|1,800
|One of largest stars
|-
|}
==See also==
*[[List of most massive stars]]
*[[List of hottest stars]]
*[[List of least massive stars]]
==References==
{{reflist}}
{{Star}}
Below is a '''list of the largest [[exoplanet]]s''' so far discovered, in terms of physical size, ordered by radius.
==List==
The sizes are listed in units of [[Jupiter radius|Jupiter radii]] ({{Jupiter radius}}, {{Jupiter radius|greek=y}}). All planets listed are larger than the largest [[planet]] in the Solar System, [[Jupiter]].
{{Expand list|date=July 2015}}
{| class="wikitable sortable"
|-
! Exoplanet
! Radius ({{Jupiter radius}}) <br/> <small> (Jupiter = 1) </small>
!class="unsortable"| Notes
|-
| [[HD 100546|HD 100546 b]]
| 6.9{{±|2.7|2.9}}<ref name="quanz2014">{{cite journal|author=Quanz, Sasch P.|display-authors=4|author2=Amara, Adam|author3=Meyer, Michael P.|author4=Kenworthy, Matthew P.|author5=Kasper, Markus|author6=Girard, Julien H.|date=2014|title=Confirmation and characterization of the protoplanet HD100546 b - Direct evidence for gas giant planet formation at 50 au|journal= Astrophysical Journal|arxiv = 1412.5173 }}</ref>
| The largest [[exoplanet]]. The planet's size puts it near the border between a giant planet and a brown dwarf.
|-
| [[HD 77065 b]]
| 3.4484<ref name="ek" />
|
|-
| [[2MASS J0839+4721 c]]
| 3.29
|
|-
| [[Gliese-758 b]]
| 3.2712<ref name="ek" />
|
|-
| [[2MASS J2126-8140]]
| 3.14
|
|-
| [[DENIS-P J082303.1-491201 b]]
| 3.055 ± 1.239<ref name="ek" /><ref name="CT-Exo-2014" />
| Most massive exoplanet known. 28.5 {{Jupiter mass}}; probably a brown dwarf. Radius estimated based on mass.<ref name="CT-Exo-2014">{{cite web |url=http://exoplanetarchive.ipac.caltech.edu/cgi-bin/DisplayOverview/nph-DisplayOverview?objname=DENIS-P+J082303.1-491201+b&type=CONFIRMED_PLANET |title=DENIS-P J082303.1-491201 b |work=[[Caltech]] |accessdate=8 March 2014}}</ref>
|-
| [[GQ Lup b]]
| 3.0<ref name=n08>Astrometric and photometric monitoring of GQ Lupi and its sub-stellar companion, Ralph Neuhäuser, Markus Mugrauer, Andreas Seifahrt, Tobias Schmidt, and Nikolaus Vogt, ''Astronomy and Astrophysics'' '''484''', #1 (2008), pp. 281–291. {{doi|10.1051/0004-6361:20078493}}. {{Bibcode|2008A&A...484..281N}}</ref>
| ~20 {{Jupiter mass}}; probably a brown dwarf. Radius estimated based on luminosity and temperature.
|-
| [[BD 26+1888 b]]
| 2.9627<ref name="ek" />
|
|-
| [[CFBDS 1458]]
| 2.932<ref name="ek" />
|
|-
| [[BD+20 2457 b]]
| 2.7773<ref name="ek" />
|
|-
| [[AS 205 Ab]]
| 2.6802<ref name="ek" />
|
|-
| [[ROXs 42Bb]]
| 2.5<ref name="EPE">{{cite web |title=All Exoplanets |url=http://exoplanet.eu/catalog/?status=&f=|date= |work=The Extrasolar Planet Encyclopedia |publisher= |accessdate=}}</ref>
| 6-15 {{Jupiter mass}}, may be a brown dwarf.
|-
| [[HD 82943 c]]
| 2.433<ref name="ek" />
|
|-
| [[HAT-P-13 c]]
| 2.4262<ref name="ek" />
|
|-
| [[HD 8673 b]]
| 2.4217<ref name="ek" />
|
|-
| [[HD 22781 b]]
| 2.39<ref name="ek" />
|
|-
| [[AB Pictoris b]]
| 2.3812<ref name="ek">{{cite web |title=Planet: All planets |url=http://www.exoplanetkyoto.org/exohtml/A_All_Exoplanets.html|date= |work=Extrasolar Planet's Catalogue |publisher=Kyoto University |accessdate=}}</ref>
|
|-
| [[WISE J1741-4642]]
| 2.32
|
|-
| [[BD+20 2457 c]]
| 2.3191<ref name="ek" />
|
|-
| [[2MASS J12074836–3900043]]
| 2.29
|
|-
| [[2MASS J2208+2921]]
| 2.29
|
|-
| [[SDSS J111010.01+011613.1]]
| 2.22
|
|-
| [[CFBDS 1458 b]]
| 2.1899
|
|-
| [[CT Cha b]]
| 2.2<ref name=substellar>Direct evidence of a sub-stellar companion around CT Cha, T. O. B. Schmidt et al., accepted for publication in ''Astronomy and Astrophysics'', {{bibcode|2008arXiv0809.2812S}}, {{arxiv|0809.2812}}.</ref>
| 11-23 {{Jupiter mass}}; is likely a brown dwarf.
|-
| [[HD 39091 b]]
| 2.1759<ref name="ek" />
|-
| [[SIMP J2154–1055]]
| 2.15
|
|-
| [[KOI-368.01]]
| 2.1<ref name="OEC">{{cite web |title=All extrasolar planets |work=Open Exoplanet Catalogue |url=http://www.openexoplanetcatalogue.com/systems/}}</ref>
|
|-
| [[XO-6b]]
| 2.07<ref name="EPE" />
| 1.9 (± 0.5) {{Jupiter mass}}; a very puffy [[Hot Jupiter]]
|-
| [[HAT-P-32b]]
| 2.037<ref name=EPE />
| 0.941 (± 0.166) {{Jupiter mass}}; a very puffy [[Hot Jupiter]]
|-
| [[WASP-17b]]
| 1.991{{±|0.08|0.58}}<ref group="note">for Case I in paper page 6, others range from 1.41 to 2.07 Jupiter radii.</ref><ref name="EPE"/><ref name="Anderson2010">{{cite journal | title=WASP-17b: An Ultra-Low Density Planet in a Probable Retrograde Orbit | url=http://iopscience.iop.org/0004-637X/709/1/159/fulltext/ | last1=Anderson | first1=D. R. | last2=Hellier | first2=C. | last3=Gillon | first3=M. | last4=Triaud | first4=A. H. M. J. | last5=Smalley | first5=B. | last6=Hebb | first6=L. | last7=Collier Cameron | first7=A. | last8=Maxted | first8=P. F. L. | last9=Queloz | first9=D. | last10=West | first10=R. G. | last11=Bentley | first11=S. J. | last12=Enoch | first12=B. | last13=Horne | first13=K. | last14=Lister | first14=T. A. | last15=Mayor | first15=M. | last16=Parley | first16=N. R. | last17=Pepe | first17=F. | last18=Pollacco | first18=D. | last19=Ségransan | first19=D. | last20=Udry | first20=S. | last21=Wilson | first21=D. M. | display-authors=1 | journal=The Astrophysical Journal | volume=709 | issue=1 | pages=159–167 | year=2010 | arxiv=0908.1553 | bibcode=2010ApJ...709..159A | doi=10.1088/0004-637X/709/1/159 }}</ref>
| Was the largest known planet in 2012. At only 0.486 {{Jupiter mass}}, this [[Hot Jupiter]] is extremely low density.
|-
| [[KOI-3681.01]]
| 2.0{{±|0.7|1}}<ref name="OEC" />
| Orbits fairly close to its 1.1{{±|0.2|0.2}} {{Solar mass}} star, with 217 day-long years.
|-
| [[KOI-680 b]]
| 1.99{{±|0.18|0.18}}<ref name="OEC" />
|
|-
| [[CVSO 30b]]
| 1.91{{±|0.21|0.21}}<ref name="EPE" />
|
|-
| [[51 Pegasi b]]
| 1.9<ref name="EPE" />
|
|-
| [[HAT-P-65b]]
| 1.89<ref name="EPE" />
|
|-
| [[HATS-23b]]
| 1.86<ref name="EPE" />
|
|-
| [[KELT-8b]]
| 1.86<ref name="EPE" />
|
|-
| [[WASP-76b]]
| 1.83<ref name="wasp" />
|
|-
| [[HAT-P-33b]]
| 1.827<ref name="EPE" />
|
|-
| [[WASP-121b]]
| 1.81<ref name="wasp" />
|
|-
| [[TRES-4b|TrES-4]]
| 1.799<ref name="binary">{{cite journal| url=http://www.mpia.de/homes/henning/Publications/daemgen.pdf| title=Binarity of transit host stars - Implications for planetary parameters| date=200| volume=498| pages=567–574 | last=Daemgen| first=S.| journal=[[Astronomy and Astrophysics]]| doi=10.1051/0004-6361/200810988| last2=Hormuth| first2=F.| last3=Brandner| first3=W.| last4=Bergfors| first4=C.| last5=Janson| first5=M.| last6=Hippler| first6=S.| last7=Henning| first7=T.| bibcode=2009A&A...498..567D|arxiv = 0902.2179 }}</ref>
|
|-
| [[KELT-12b]]
| 1.79<ref name="OEC" />
|
|-
| [[HATS-26b]]
| 1.75<ref name="EPE" />
|
|-
| [[WASP-12b]]
| 1.736<ref name="wasp" />
|
|-
| [[HAT-P-46b]]
| 1.73<ref name="EPE" />
|
|-
| [[WASP-94 Ab]]
| 1.72<ref name="wasp" />
|
|-
| [[KELT-4Ab]]
| 1.706<ref name="OEC" />
|
|-
| [[WASP-79b]]
| 1.7<ref name="EPE" />
|
|-
| [[WASP-78b]]
| 1.7<ref name=wasp>{{cite web|url=http://wasp-planets.net/wasp-planets/|title=WASP Planets|work=SuperWASP|accessdate=2016-01-26}}</ref>
|
|-
| [[1RXS 1609b]]
| 1.7<ref name="EPE" />
|
|-
| [[WASP-88b]]
| 1.7<ref name="wasp" />
|
|-
|-
|}
{| class="wikitable sortable"
|+'''The following well-known exoplanets are listed for the purpose of comparison.'''
|-
! Exoplanet
! Radius ({{Jupiter radius}}) <br/> <small> (Jupiter = 1) </small>
!class="unsortable"| Notes
|-
| [[Kepler-12b]]
| 1.695<ref name="EPE" />
|
|-
| [[Kepler-447b]]
| 1.65
|
|-
| [[beta Pic b]]
| 1.65
|
|-
| [[OGLE2-TR-L9b]]
| 1.614<ref name="OEC" />
|
|-
| [[PSO J318.5-22]]
| 1.53
|
|-
| [[WASP-103b]]
| 1.528
|
|-
| [[Kepler-13b]]
| 1.51<ref name="OEC" />
|
|-
| [[HAT-P-8b]]
| 1.5
|
|-
| [[WASP-71b]]
| 1.5
|
|-
| [[Kepler-854b]]
| 1.5
|
|-
| [[WASP-33b]]
| 1.497
|
|-
| [[Kepler-7b]]
| 1.478
|
|-
| [[Kepler-5b]]
| 1.431
|
|-
| [[Kepler-8b]]
| 1.419
|
|-
| [[TrES-3]]
| 1.341
|
|-
| [[XO-4b]]
| 1.34
|
|-
| [[TrES-2b]]
| 1.272
|
|-
| [[OGLE-TR-10b]]
| 1.26
|
|-
| [[Kepler-39b]]
| 1.22
|One of the most massive exoplanets known.
|-
| [[Kepler-418b]]
| 1.2
|
|-
| [[Kappa And b]]
| 1.2
|
|-
| [[OGLE-TR-182b]]
| 1.13
|
|-
|- style="background:pink;" class="sortbottom"
| [[Jupiter]]
| 69,911 km <ref>{{cite web |url= http://www.universetoday.com/36649/planets-in-order-of-size/ |title= The Planets in Our Solar System in Order of Size |author= Elizabeth Howell |date= 21 April 2014 |publisher= Universe Today }}</ref>
| Largest [[Solar System planets|planet]] in the [[Solar System]], by radius and volume.<ref>{{cite web |url= http://www.universetoday.com/15453/what-is-the-biggest-planet-in-the-solar-system/ |title= What is the Biggest Planet in the Solar System? |author= Jerry Coffey |date= 8 July 2008 |publisher= Universe Today }}</ref> <br/> <small> Reported for reference </small>
|-
|}
== Timeline of largest exoplanet recordholders ==
{|class=wikitable
|-
! Planet
! Size ({{Jupiter radius}})
! Date
!class="unsortable"| Notes
|-
| {{nowrap|[[HD 100546 b]]}}
| 6.9<ref name="NASA">{{cite web|url=http://exoplanetarchive.ipac.caltech.edu/cgi-bin/TblView/nph-tblView?app=ExoTbls&config=planets&constraint=pl_pnum%20%3E1 |title=Confirmed Planets|author=NASA|work=NASA Website|publisher=NASA Exoplanet Archive}}</ref>
| 2015—
|
|-
| {{nowrap|[[HAT-P-32b]]}}
| 2.02
| 2013—2015
| [[CT Cha b]] may be larger at over 2.2 Jupiter radii, but its status as a planet or brown dwarf is unconfirmed.
|-
| {{nowrap|[[WASP-17b]]}}
| 1.991
| 2012—2013
|
|-
| {{nowrap|[[WASP-12b]]}}
| 1.83
| 2009—2012
|
|-
| {{nowrap|[[TRES-4b]]}}
| 1.67
| 2007—2009
| This planet has a density of 0.2 g/cm<sup>3</sup>, about that of balsa wood, less than Jupiter's 1.3g/cm<sup>3</sup> It was succeeded by WASP-17b as the largest exoplanet.<ref>{{cite news |url= http://www.space.com/4151-largest-exoplanet-discovered.html |title= Largest Known Exoplanet Discovered |author= Ker Than |date= 6 August 2007 |publisher= Space.com }}</ref><ref>{{cite web |url= http://www.keckobservatory.org/recent/entry/keck_confirms_largest_exoplanet_to_date |title= Keck Confirms Largest Exoplanet To Date |date= 6 August 2007 |author= California Institute of Technology |publisher= W.M. Keck Observatory }}</ref>
|-
| {{nowrap|[[HD 209458 b]]}}
| 1.3
| —2007
| This was the first exoplanet whose size was determined.<ref>{{cite journal |journal= Scientific American |author1=Laurance R. Doyle |author2=Hans-Jörg Deeg |author3=Timothy M. Brown |title= Searching for Shadows of Other Earths |url= http://www.iac.es/proyecto/tep/papers2000/SciAmtransit.pdf |date= September 2000 |pages= 59–65 |doi= 10.1038/scientificamerican0900-58 |pmid= 10976467 |volume=283}}</ref>
|-
|}
== See also ==
* [[List of largest cosmic structures]]
* [[List of largest galaxies]]
* [[List of largest nebulae]]
* [[List of largest stars]]
==Notes==
{{reflist|group=note}}
== References ==
{{reflist}}
{{Exoplanet}}
{{Original research|date=October 2015}}
[[File:Nursery of New Stars - GPN-2000-000972.jpg|300px|thumb|[[NGC 604]], one of largest [[nebula]]e ([[H II region]]) is localed in the [[Triangulum Galaxy]]<br>''(viewed by the [[Hubble Space Telescope]])''.]]
Below is a '''list of the largest [[nebula]]e''' so far discovered, ordered by size.
==List==
{{expand list|date=November 2014}}
{| class="wikitable sortable"
|+'''List of the largest H II regions'''
|-
! style="background: {{star-color|WN}};" | H II region
! style="background:#ffdead;"| Size ([[light year|ly]]/[[parsec|pc]])
! Type
!class="unsortable"| Notes
|-
| [[NGC 604]]
| {{convert|1,520|ly|pc|abbr=on}}<ref>distance × sin( diameter_angle / 2 ) = 760 ly. radius</ref>
| [[H II region]]
| Located in the [[Triangulum Galaxy]]
|-
| [[Gum Nebula]]
| {{convert|1,100|ly|pc|abbr=on}}
| Emission Nebula
|
|-
| [[N44 (emission nebula)|N44]]
| {{convert|1,000|ly|pc|abbr=on}}<ref name="roses">{{cite web |url = http://www.eso.org/public/news/eso0332/ |title = Roses in the Southern Sky |date = 3 November 2003 |publisher = ESO |accessdate = 7 May 2012}}</ref>
| Emission Nebula
|
|-
| [[Tarantula Nebula]]
| {{convert|600x652|ly|pc|abbr=on}}<ref name="Lebouteilleretal2008">{{Cite journal
| bibcode = 2008ApJ...680..398L
| title = Chemical Composition and Mixing in Giant H II Regions: NGC 3603, 30 Doradus, and N66
| date = June 2008
| journal = The Astrophysical Journal
| volume = 680
| issue = 1
| pages = 398–419
| doi = 10.1086/587503
| display-authors = 4
| author = Lebouteiller, V.
| author2 = Bernard-Salas, J.
| author3 = Brandl, B.
| author4 = Whelan, D. G.
| author5 = Wu, Yanling
| author6 = Charmandaris, V.
| author7 = Devost, D.
| author8 = Houck, J. R.
|arxiv = 0710.4549 }}</ref>
| [[H II region]]
| Most active starburst region in the Local Group
|-
| [[N119]]
| {{convert|430x570|ly|pc|abbr=on}}
| [[H II region]]
| Peculiar S-shape
|-
| [[Carina Nebula]]
| {{convert|460|ly|pc|abbr=on}}<ref name="Atlas">{{cite web|title=NGC 3372 - The Eta Carinae Nebula|work=Atlas of the Universe|url=http://www.atlasoftheuniverse.com/nebulae/ngc3372.html|accessdate=2013-10-01}}</ref>
| [[H II region]]
| Nearest giant H II region to Earth
|-
| [[RCW 49]]
| {{convert|350|ly|pc|abbr=on}}
| [[H II region]]
|
|-
| [[H II region|N70]]
| {{convert|300|ly|pc|abbr=on}}
| [[H II region]]
| The N 70 Nebula, in the Large Magellanic Cloud has a shell structure and is really a bubble in space. It is a "Super Bubble".
|-
| [[Barnard's Loop]]
| {{convert|100x300|ly|pc|abbr=on}}
| [[H II region]]
|
|-
| [[Cygnus Loop]]
| {{convert|125x210|ly|pc|abbr=on}}
| [[Supernova remnant|SNR]]
|
|-
| [[Eagle Nebula]]
| {{convert|110x140|ly|pc|abbr=on}}
| [[H II region]]
|
|-
| [[Rosette Nebula]]
| {{convert|130|ly|pc|abbr=on}}
| [[H II region]]
|
|-
| [[Lagoon Nebula]]
| {{convert|40x110|ly|pc|abbr=on}}
| [[H II region]]
|
|-
| [[Veil Nebula]]
| {{convert|100|ly|pc|abbr=on}}
| [[Supernova remnant]]
|
|}
===List of largest H I regions===
===List of largest lyman-alpha blobs===
[[File:Lyman-alpha blob LAB-1.jpg|250px|thumb|Polarized image of [[Lyman-alpha blob 1]], shown as the faint, green gas cloud]]
{| class="wikitable sortable"
|+'''List of the largest lyman-alpha blobs'''
|-
! style="background: {{star-color|WC}};" | Lyman-alpha blobs
! style="background:#ffdead;"| Size ([[light year|ly]]/[[parsec|pc]])
! Type
!class="unsortable"| Notes
|-
|LAB Giant Concentration<br />(coinciding with [[EQ J221734.0+001701]])
| {{convert|200,000,000|ly|pc|abbr=on}}<ref name=NG>{{cite web|last=Ravilious|first=Kate|title=Giant "Blob" is Largest Thing in Universe|url=http://news.nationalgeographic.com/news/2006/07/060731-giant-blob.html|publisher=National Geographic News|accessdate=June 23, 2011}}</ref>
| complex of [[Lyman alpha blob|LαB]]s
| Also on record as one of the [[List of largest cosmic structures|largest structures]] in the universe.
|-
|[[Lyman-alpha blob 1]]
| {{convert|300,000|ly|pc|abbr=on}}<ref name="ESO">{{cite news|title=Giant Space Blob Glows from Within|url=http://www.eso.org/public/news/eso1130/|accessdate=18 August 2011|newspaper=ESO Press Release|date=17 August 2011}}</ref>
| [[Lyman alpha blob|LαB]]
| Largest blob in the LAB Giant Concentration
|-
|[[Himiko (Lyman-alpha blob)|Himiko Gas Cloud]]
| {{convert|55,000|ly|pc|abbr=on}}<ref name="space.com">{{cite news|url=http://www.space.com/scienceastronomy/090422-space-blob.html|title=Giant Mystery Blob Discovered Near Dawn of Time|last=Hsu|first=Jeremy|date=2009-04-22|publisher=SPACE.com|accessdate=2009-04-24}}</ref>
| intergalactic cloud<br />(possible [[Lyman-alpha blob|LαB]])
| One of the most massive lyman-alpha blobs known
|}
===List of largest High-velocity clouds===
{| class="wikitable sortable"
|+'''List of the largest High-velocity clouds'''
|-
! High-velocity clouds
! style="background:#ffdead;"| Size ([[light year|ly]]/[[parsec|pc]])
! Type
!class="unsortable"| Notes
|-
| [[NGC 262]] Halo Cloud
| {{convert|1,300,000|ly|pc|abbr=on}}
| [[H I region]]
| Spiral nebula surrounding NGC 262. NGC 262 is also [[List of largest galaxies|one of the largest known galaxies]].
|-
| [[Leo Ring]]
| {{convert|650,000|ly|pc|abbr=on}}<ref name=CFHT-LeoRing-2010>{{cite web |url= http://www.cfht.hawaii.edu/en/news/LeoRing/ |title= The mysterious Leo giant gas ring explained by a billion year old collision between two galaxies |date= 2010 |author1=Léo Michel-Dansa |author2=Pierre-Alain Duc |publisher= Canada France Hawaii Telescope }}</ref>
| HVC
|
|-
| [[Magellanic Stream]]
| {{convert|600,000|ly|pc|abbr=on}}
| complex of [[high velocity cloud|HVC]]s
| Connects the [[Large Magellanic Cloud|Large]] and [[Small Magellanic Cloud|Small]] [[Magellanic clouds]]; extends across 180° of the sky.
|-
| [[HVC 127-41-330]]
| {{convert|20,000|ly|pc|abbr=on}}<ref name="simon">{{cite paper |author = Josh Simon | coauthors = | title = Dark Matter in Dwarf Galaxies: Observational Tests of the Cold Dark Matter Paradigm on Small Scales | version = | publisher = | date = 2005 | url = http://www.astro.caltech.edu/~jsimon/thesis/jdsthesis.pdf | accessdate = |archivedate=September 13, 2006 |archiveurl=https://web.archive.org/web/20060913084945/http://www.astro.caltech.edu/~jsimon/thesis/jdsthesis.pdf |dead-url=yes }}</ref>
| HVC
|
|-
| [[Smith's Cloud]]
| {{convert|3,300x9,800|ly|pc|abbr=on}}<ref name=lockman>{{cite journal
| last1 = Lockman
| first1 = Felix J.
| last2 = Benjamin
| first2 = Robert A.
| last3 = Heroux
| first3 = A. J.
| last4 = Langston
| first4 = Glen I.
| title = The Smith Cloud: A High-Velocity Cloud Colliding with the Milky Way
| journal = The Astrophysical Journal
|date=May 2008
| volume = 679
| issue = 1
| pages = L21
| format = PDF
| doi = 10.1086/588838
| bibcode = 2008ApJ...679L..21L
| arxiv = 0804.4155
| url = http://iopscience.iop.org/1538-4357/679/1/L21/pdf/22647.pdf
| accessdate = April 3, 2012
}}</ref>
| [[High velocity cloud|HVC]]
| Extends about 20° of the sky
|-
|}
===List of largest star clusters===
{{expand list|date=June 2017}}
{| class="wikitable sortable"
|+'''List of the largest star clusters'''
|-
! Star clusters
! style="background:#ffdead;"| Size ([[light year|ly]]/[[parsec|pc]])
! Type
!class="unsortable"| Notes
|-
| [[NGC 206]]
| {{convert|800|ly|pc|abbr=on}}
|
|
|-
| [[Sagittarius Star Cloud]]
| {{convert|600|ly|pc|abbr=on}}
|
|
|-
| [[NGC 2419]]
| {{convert|520|ly|pc|abbr=on}}
|
| The largest known [[globular cluster]]
|-
| [[NGC 121]]
| {{convert|350|ly|pc|abbr=on}}
|
|
|-
| [[Palomar 12]]
| {{convert|324|ly|pc|abbr=on}}
|
|
|-
| [[Terzan 7]]
| {{convert|320|ly|pc|abbr=on}}
|
|
|-
| [[Laevens 1]]
| {{convert|320|ly|pc|abbr=on}}
|
|
|-
| [[Messier 54]]
| {{convert|306|ly|pc|abbr=on}}
|
|
|-
| [[NGC 339]]
| {{convert|238|ly|pc|abbr=on}}
|
|
|-
|-
| [[Messier 3]]
| {{convert|180|ly|pc|abbr=on}}
|
|
|-
| [[Messier 15]]
| {{convert|176|ly|pc|abbr=on}}
|
|
|-
| [[Messier 2]]
| {{convert|174.6|ly|pc|abbr=on}}
|
|
|-
| [[Omega Centauri]]
| {{convert|172|ly|pc|abbr=on}}
|
|
|-
| [[Messier 13]]
| {{convert|168|ly|pc|abbr=on}}
|
|
|-
| [[Messier 5]]
| {{convert|160|ly|pc|abbr=on}}
|
|
|-
| [[Palomar 5]]
| {{convert|152|ly|pc|abbr=on}}
|
|
|-
| [[Messier 19]]
| {{convert|140|ly|pc|abbr=on}}
|
|
|-
| [[Messier 75]]
| {{convert|134|ly|pc|abbr=on}}
|
|
|-
| [[47 Tucanae]]
| {{convert|120|ly|pc|abbr=on}}
|
|
|-
| [[Messier 68]]
| {{convert|106|ly|pc|abbr=on}}
|
|
|-
| [[Messier 14]]
| {{convert|100|ly|pc|abbr=on}}
|
|
|-
| [[Messier 22]]
| {{convert|100|ly|pc|abbr=on}}
|
|
|}
==See also==
* [[List of largest cosmic structures]]
* [[List of largest galaxies]]
* [[List of largest stars]]
* [[List of largest planets]]
==References==
{{reflist}}
{{Nebula}}
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