List of largest stars

Relative sizes of the planets in the Solar System and several well-known stars:

Below is an ordered list of the largest stars currently known by radius. The unit of measurement used is the radius of the Sun (approximately 695,700 km; 432,288 mi).

The exact order of this list is very incomplete, as great uncertainties currently remain, especially when deriving various important parameters used in calculations, such as stellar luminosity and effective temperature. Often stellar radii can only be expressed as an average or within a large range of values. Values for stellar radii vary significantly in sources and throughout the literature, mostly as the boundary of the very tenuous atmosphere (opacity) greatly differs depending on the wavelength of light in which the star is observed.

Radii of several stars can be directly obtained by stellar interferometry. Other methods can use lunar occultations or from eclipsing binaries, which can be used to test other indirect methods of finding true stellar size. Only a few useful supergiant stars can be occulted by the Moon, including Antares and Aldebaran. Examples of eclipsing binaries include Epsilon Aurigae, VV Cephei, and HR 5171.

Caveats

UY Scuti as seen in visible light.

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

  • Largest stars are usually expressed in units of the solar radius (R☉), where 1.00 R☉ equals 695,700 kilometres.
  • Stellar radii or diameters are usually only approximated using Stefan–Boltzmann law for the deduced stellar luminosity and effective surface temperature;
  • Stellar distances, and their errors, for most, remain uncertain or poorly determined;
  • Many supergiant stars have extended atmospheres and many are embedded within opaque dust shells, making their true effective temperatures highly uncertain;
  • Many extended supergiant atmospheres also significantly change in size over time, regularly or irregularly pulsating over several months or years as variable stars. This makes adopted luminosities poorly known and may significantly change the quoted radii;
  • Other direct methods for determining stellar radii, rely on lunar occultations or from eclipses in binary systems. This is only possible for a very small number of stars;
  • Based on various theoretical evolutionary models, few stars will exceed 1,500–2,000 times the Sun (roughly 3,715 K and Mbol = −9). Such limits maybe also depend on the stellar metallicity.[1]

Extragalactic large stars

In this list are some examples of more distant extragalactic stars, which may have slightly different properties and natures than the currently largest known stars in the Milky Way:

  • Some red supergiants in the Magellanic Clouds are suspected to have slightly different limiting temperatures and luminosities. Such stars may exceed accepted limits by undergoing large eruptions or change their spectral types over just a few months. Humphreys et al., for example, calculates the maximum size for a Magellanic cloud star as ~2,600 R☉.
  • A survey of the Magellanic Clouds has catalogued many red supergiants, where more than 50 of them exceed 700 R☉ (490,000,000 km; 3.3 AU; 300,000,000 mi). Largest of these is about 1,200–1,300 R☉.[2]

List

This list is incomplete; you can help by expanding it.
List of the largest stars
Star name Solar radii
(Sun = 1)		 Method[lower-alpha 1] Notes
Orbit of Saturn1,940–2,169Reported for reference
UY Scuti1,708 ± 192[3]ADThe quoted size was based on an angular diameter and distance of 2.9 kpc. Gaia Data Release 2 suggests a much closer distance and consequently smaller radius.
WOH G641,540[4]–1,730[5]L/TeffThis would be the largest star in the LMC, but is unusual in position and motion and might still be a foreground halo giant.
RW Cephei 1,535[6][7]L/TeffRW 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 1,530–1,580[8] (–2,550) [9]L/TeffVery uncertain parameters for an unusual star with strong radio emission. The spectrum is variable but apparently the luminosity is not.
HD 1431831,480[10]–1,830[11]L/Teff
VY Canis Majoris1,420 ± 120[12]ADThe size of VY CMa was revised in 2012 through newly improved measurements[13] which result this value being the highest among well-characterized stars.[14] Other stars could be larger but they could have less accurate radius estimates.
KY Cygni 1,420–2,850 [1]L/TeffThe upper estimate is due to an unusual K-band measurement and thought to be an artifact of a reddening correction error, and is thought to be against stellar evolutionary theory. The lower estimate is consistent with other stars in the same survey and with theoretical models.
AH Scorpii1,411 ± 124[3]ADAH 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.
RSGC1-F021,398[15]L/Teff
IRAS 04509-69221,360[16]L/Teff
RSGC1-F011,335[15]L/Teff
HR 5171 A1,315 ± 260,[17] 1,575 ± 400[18]ADHR 5171 A is a highly distorted star in a close binary system, losing mass to the secondary, and is also variable in temperature, thus probably also in diameter. Traditionally, it is considered as the largest known yellow hypergiant, although the latest research suggests it is a red supergiant with a radius of 1,490 ± 540 R☉.[19]
SMC 181361,310[2]Largest star in the Small Magellanic Cloud
IRAS 05280-69101,260[16] - 1,738[20]L/Teff
Mu Cephei (Herschel's "Garnet Star")1,260[21]Prototype of the obsolete class of the Mu Cephei variables and also the reddest star in the night sky in terms of the B-V color index.[22] Other recent estimates range from 650 R☉[23] to 1,420 R☉[1]
LMC 1360421,240[2]
BI Cygni1,240[1]L/Teff
Westerlund 1-2371,233[9]L/Teff
SMC 50921,220[2]
S Persei1,212 ± 124[24]AD & L/TeffA red hypergiant localed in the Perseus Double Cluster. A large radius of 1,230 R☉ is due to an unusual K-band measurement and thought to be an artifact of a reddening correction error. A small radius of 780 R☉ is consistent with other stars in the same survey and with theoretical models.[1]
LMC 1754641,200[2]
LMC 1357201,200[2]
IRC-104141,200[25]IRC -10414 is a rare red supergiant companion to WR 114 that has a bow shock.
PZ Cassiopeiae1,190–1,940[1]L/TeffThe 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, and the intermediate ones have been obtained refining the distance to this star, and thus its parameters.[26]
SMC 698861,190[2]
NML Cygni1,183[27]L/Teff
RSGC1-F051,177[15]L/Teff
EV Carinae1,168[28]-2,880[29]L/Teff
RSGC1-F031,168[15]L/Teff
LMC 1192191,150[2]
RSGC1-F081,146[15]L/Teff
BC Cygni1,140[1]-1,230[21]L/TeffBC Cyg is calculated to vary in size from 856 R☉ to 1,553 R☉.[30]
MY Cephei1,134[31]L/TeffOne of the coolest known red supergiants.
SMC 108891,130[2]
VX Sagittarii1,120 - 1,550[32]L/TeffVX Sgr is a pulsating variable calculated to vary in size from 1,350 R☉ to 1,940 R☉.[33]
LMC 1414301,110[2]
IRAS 04516-69021,100[16]L/Teff
LMC 1757461,100[2]
RSGC1-F131,098[15]L/Teff
RT Carinae1,090[1]L/Teff
RSGC1-F041,082[15]L/Teff
LMC 1747141,080[2]
LMC 681251,080[2]
SMC 494781,080[2]
SMC 201331,080[2]
V396 Centauri1,070[1]L/Teff
SMC 89301,070[2]
Orbit of Jupiter1,064–1,173 Reported for reference
HV 114231,060–1,220[34]L/TeffHV 11423 is variable in spectral type (observed from K0 to M5), thus probably also in diameter. In October 1978, it was a star of M0I type.
CK Carinae1,060[1]L/Teff
SMC 258791,060[2]
VV Cephei A1,050[35] - 1,900[1]VV Cep A is a highly distorted star in a close binary system, losing mass to the secondary for at least part of its orbit. Data from the most recent eclipse has cast additional doubt on the accepted model of the system. It is among the largest stars visible to the naked eye.
LMC 1422021,050[2]
LMC 1461261,050[2]
LMC 679821,040[2]
U Lacertae1,022[36][37]L/Teff
RSGC1-F111,015[15]L/Teff
W Persei1,011[9]L/Teff
LMC 1438771,010[2]
KW Sagittarii1,009[3]-1,460[1]AD & L/TeffMargin of possible error: ±142 R☉.[3]
RSGC1-F121,005[9]L/Teff
Progenitor of SN 2017eaw1,000–2,000[38]Localed in NGC 6946
SMC 46497990[2]
LMC 140296990[2]
RSGC1-F09986[15]L/Teff
NR Vulpeculae980[1]L/Teff
SMC 12322980[2]
LMC 177997980[2]
SMC 59803970[2]
Westerlund 1-20965[9]L/Teff
GCIRS 7960[39]–1,000[40]ADAt the galactic center. Margin of possible error: ±92 R☉[39] or ±150 R☉.[40]
Betelgeuse (Alpha Orionis)955±217[41]ADStar with the third largest apparent size after R Doradus and the Sun. Other estimates range from 887 ± 203 R☉[42] to 1,180 R☉[43]
SMC 50840950[2]
J004424.94+412322.3945–1,300[44]L/TeffLocated in the Andromeda Galaxy.
RSGC1-F10931[15]L/Teff
S Cassiopeiae930[45][46]
IX Carinae920[1]L/Teff
HV 2112916[47]L/TeffMost likely candidate for a Thorne-Zytkow Object.
RSGC1-F07910[15]L/Teff
LMC 54365900[2]
IRAS 04498-6842900[48]–1,660[16]L/Teff
NSV 25875891[27]L/Teff
LMC 109106890[2]
RSGC1-F06885[15]L/Teff
LMC 116895880[2]
SMC 30616880[2]
LMC 64048880[2]
IRAS 05558-7000880[16]L/Teff
V437 Scuti874[27]L/Teff
IRAS 04407-7000870[16]L/Teff
IRAS 05329-6708870[16]L/Teff
V602 Carinae860[1]–1,050[49]L/Teff & ADMargin of possible error: ±165 R☉.[49]
J004047.82+410936.4860[44]L/TeffLocaled in the Andromeda Galaxy
J004428.71+420601.6860[44]L/TeffLocaled in the Andromeda Galaxy
V669 Cassiopeiae859[27]L/Teff
SMC 55681850[2]
SMC 15510850[2]
LMC 61753830[2]
LMC 62090830[2]
SMC 11709830[2]
V1185 Scorpii830[27]L/Teff
LMC 142199810[2]
IRAS 05294-7104810[16]L/Teff
IRAS 05402-6956800[16]L/Teff
LMC 134383800[2]
Eta Carinae A (Tseen She)800[50]Previously thought to be the most massive single star, but in 2005 it was realized to be a binary system. During the Great Eruption, the size was as large as 1,400 R☉.[51]
V441 Persei799[9]L/Teff
BU Persei795[9]L/Teff
IRAS 05298-6957790[16]L/Teff
BO Carinae790[1]L/Teff
LMC 142907790[2]
J004359.94+411330.9785[44]L/TeffLocaled in the Andromeda Galaxy
SU Persei780[1]L/TeffIn the Perseus Double Cluster
RS Persei770[52]–1,000[1]AD & L/TeffIn the Perseus Double Cluster. Margin of possible error: ±30 R☉.[52]
AV Persei770[1]L/TeffIn the Perseus Double Cluster
V355 Cephei770[1]L/TeffMauron et al. 2011 derive 37,000 L☉, which implies a size around 300 R☉.[36]
J004124.80+411634.7760[44]L/TeffLocaled in the Andromeda Galaxy
V915 Scorpii760[53][54]L/Teff
S Cephei760[55]AD
YZ Persei758[9]L/Teff
J004447.08+412801.7755[44]L/TeffLocaled in the Andromeda Galaxy
GP Cassiopeiae751[9]L/Teff
Outer limits of the asteroid belt750–900 Reported for reference
SMC 11939750[2]
HD 303250750[1]L/Teff
V382 Carinae747[56]The brightest yellow hypergiant in the night sky, one of the rarest types of star. Other estimate ranges of 600 R☉ to 1,100 R☉.[57]
RU Virginis740[58]L/Teff
LMC 137818740[2]
SMC 48122740[2]
IRAS 04545-7000730[16]L/Teff
IRAS 05003-6712730[16]L/Teff
SMC 56732730[2]
KK Persei724[9]L/Teff
V648 Cassiopeiae710[1]L/Teff
XX Persei710[9]L/TeffLocated in the Perseus Double Cluster and near the border with Andromeda.
TV Geminorum620–710[59] (–770)[1]L/Teff
HD 179821704[60]A yellow hypergiant, although most authors consider it as a supergiant, a protoplanetary nebula or a post-AGB star with a luminosity of only 16,000 L☉.
J004255.95+404857.5700[44]L/TeffLocaled in the Andromeda Galaxy
J003950.98+405422.5700[61]L/TeffLocaled in the Andromeda Galaxy
LMC 169754700[2]
LMC 65558700[2]
V528 Carinae700[1]L/Teff
RSGC1-F14700[15]L/Teff
The following well-known stars are listed for the purpose of comparison.
V354 Cephei690[36]-1,520[1]L/Teff
Antares A (Alpha Scorpii A)680[62]ADThis star appears to vary its size by 165 R☉. Older estimates have given radii over 800 R☉,[63][64] but some are likely to have been affected by asymmetry of the atmosphere and the narrow range of infrared wavelengths observed.[62]
HR 5171 Ab650±150[18]ADCompanion of HR 5171 A.
CE Tauri587–593[65] (–608[66])ADSecond reddest star in the night sky.[22] Can be occulted by the Moon, allowing accurate determination of its apparent diameter.
CW Leonis500[67]–700[68]L/TeffCW Leonis is one of the mistaken identities as the claimed planet "Nibiru" or "Planet X", due to its brightness as it approaches 1st magnitude. Other estimates range from 390 R☉[67] to 826 R☉.[27]
Rho Cassiopeiae400–500[69]Yellow hypergiant, one of the rarest types of a star.
R Leporis (Hind's "Crimson Star")400[70]–535[71]Margin of possible error: ±90 R☉.[70]
V509 Cassiopeiae400–900[72]Yellow hypergiant, one of the rarest types of a star.
Inner limits of the asteroid belt380 Reported for reference
V838 Monocerotis380 (in 2009)[73]A short time after the outburst V838 Mon was measured at 1,570 ± 400 R☉.[74] However the distance to this "L-type supergiant", and hence its size, have since been reduced and it proved to be a transient object that shrunk about four-fold over a few years. Like CW Leo, it has been erroneously portrayed as "Nibiru" or "Planet X" (see above).
R Doradus370±50[75]Star with the second largest apparent size after the Sun.
Tail of Comet Hyakutake360Reported for reference
IRC +10420357[76]–1,342[27]L/TeffA yellow hypergiant that has increased its temperature into the LBV range.
The Pistol Star340[77]Blue hypergiant, among the most massive and luminous stars known.
Mira A (Omicron Ceti)332–402[78]ADPrototype Mira variable. De beck et al. 2010 calculates 541 R☉.[27]
La Superba (Y Canum Venaticorum)307[27]–390[79]L/TeffReferred to as La Superba by Angelo Secchi. Currently one of the coolest and reddest stars.
Orbit of Mars297–358Reported for reference
Alpha Herculis (Ras Algethi)284±60[80]The estimate ranges from 264 R☉ to 303 R☉[80]
Sun's red giant phase256[81]The core hydrogen would be exhausted in 5.4 billion years. In 7.9 billion years, The Sun would reach the tip of the red-giant branch of the Hertzsprung–Russell diagram. (see below)
Reported for reference
Orbit of Earth215 (211–219)Reported for reference
Deneb (Alpha Cygni)203±17[82]Prototype Alpha Cygni variable.
Solar System Habitable Zone200–520[83] (uncertain)Reported for reference
Orbit of Venus154–157Reported for reference
Epsilon Aurigae A (Almaaz)143–358[84]ε Aur was incorrectly claimed in 1970 as the largest star with a size between 2,000 R☉ and 3,000 R☉,[85] even though it later turned out not to be an infrared light star but rather a dusk torus surrounding the system.
S Doradus100–380[86]Prototype S Doradus variable, even though P Cygni was the first discovered.
Peony Star92[87]Candidate for most luminous star in the Milky Way.
Rigel A (Beta Orionis A)78.9[88]–115[89]Margin of possible error: ±7.4 R☉.[88]
Canopus (Alpha Carinae)71±4[90]Second brightest star in the night sky.
Orbit of Mercury66–100Reported for reference
LBV 1806-2045–145[91]L/TeffFormerly a candidate for the most luminous star in the Milky Way with 40 million L☉,[92] but the luminosity has been revised later only 2–5 million L☉.[93][94]
Aldebaran (Alpha Tauri)44.13±0.84[95]AD
Polaris (Alpha Ursae Minoris)37.5[96]The current northern pole star.
R136a128.8[97]–35.4[98]Also on record as the most massive and luminous star known (265 - 315 M☉ and 8.71 million L☉).
Arcturus (Alpha Boötis)25.4±0.2[99]Brightest star in the northern hemisphere.
HDE 22686820–22[100]The supergiant companion of black hole Cygnus X-1. The black hole is 500,000 times smaller than the star.
VV Cephei B13[101]–25[102]The B-type main sequence companion of VV Cephei A.
Sun's helium burning phase10After the red-giant branch the Sun has approximately 120 million years of active life left.
Reported for reference
Sun1The largest object in the Solar System.
Reported for reference
  1. ↑ AD: radius determined from angular diameter and distance
    L/Teff: radius calculated from bolometric luminosity and effective temperature

See also

References

  1. 1 2 3 4 5 6 7 8 9 10 11 12 13 14 15 16 17 18 19 20 21 22 23 24 25 Table 4 in Levesque, Emily M.; Massey, Philip; Olsen, K. A. G.; Plez, Bertrand; Josselin, Eric; Maeder, Andre; Meynet, Georges (2005). "The Effective Temperature Scale of Galactic Red Supergiants: Cool, but Not as Cool as We Thought". The Astrophysical Journal. 628 (2): 973–985. arXiv:astro-ph/0504337. Bibcode:2005ApJ...628..973L. doi:10.1086/430901.
  2. 1 2 3 4 5 6 7 8 9 10 11 12 13 14 15 16 17 18 19 20 21 22 23 24 25 26 27 28 29 30 31 32 33 34 35 36 37 38 39 40 41 42 43 44 45 46 Levesque, Emily M.; Massey, Philip; Olsen, K.A.G.; Plez, Bertrand; Meynet, Georges; Maeder, Andre (2006). "The Effective Temperatures and Physical Properties of Magellanic Cloud Red Supergiants: The Effects of Metallicity". The Astrophysical Journal. 645 (2): 1102–1117. arXiv:astro-ph/0603596. Bibcode:2006ApJ...645.1102L. doi:10.1086/504417.
  3. 1 2 3 4 Arroyo-Torres, B; Wittkowski, M; Marcaide, J. M; Hauschildt, P. H (June 2013). "The atmospheric structure and fundamental parameters of the red supergiants AH Scorpii, UY Scuti, and KW Sagittarii". Astronomy & Astrophysics. 554 (A76): A76. arXiv:1305.6179. Bibcode:2013A&A...554A..76A. doi:10.1051/0004-6361/201220920.
  4. ↑ Levesque, Emily M; Massey, Philip; Plez, Bertrand; Olsen, Knut A. G (June 2009). "The Physical Properties of the Red Supergiant WOH G64: The Largest Star Known?". Astronomical Journal. 137 (6): 4744. arXiv:0903.2260. Bibcode:2009AJ....137.4744L. doi:10.1088/0004-6256/137/6/4744.
  5. ↑ Ohnaka, K.; Driebe, T.; Hofmann, K. H.; Weigelt, G.; Wittkowski, M. (2009). "Resolving the dusty torus and the mystery surrounding LMC red supergiant WOH G64". Proceedings of the International Astronomical Union. 4: 454. Bibcode:2009IAUS..256..454O. doi:10.1017/S1743921308028858.
  6. ↑ Humphreys, R. M. (1978). "Studies of luminous stars in nearby galaxies. I. Supergiants and O stars in the Milky Way". The Astrophysical Journal Supplement Series. 38: 309. Bibcode:1978ApJS...38..309H. doi:10.1086/190559.
  7. ↑ Davies, Ben; Kudritzki, Rolf-Peter; Figer, Donald F. (2010). "The potential of red supergiants as extragalactic abundance probes at low spectral resolution". Monthly Notices of the Royal Astronomical Society. 407 (2): 1203. arXiv:1005.1008. Bibcode:2010MNRAS.407.1203D. doi:10.1111/j.1365-2966.2010.16965.x.
  8. ↑ Wright, Nicholas J; Wesson, Roger; Drew, Janet E; Barentsen, Geert; Barlow, Michael J; Walsh, Jeremy R; Zijlstra, Albert; Drake, Jeremy J; Eislöffel, Jochen; Farnhill, Hywel J (2014). "The ionized nebula surrounding the red supergiant W26 in Westerlund 1". Monthly Notices of the Royal Astronomical Society: Letters. 437 (1): L1. arXiv:1309.4086. Bibcode:2014MNRAS.437L...1W. doi:10.1093/mnrasl/slt127.
  9. 1 2 3 4 5 6 7 8 9 10 11 Fok, Thomas K. T; Nakashima, Jun-ichi; Yung, Bosco H. K; Hsia, Chih-Hao; Deguchi, Shuji (2012). "Maser Observations of Westerlund 1 and Comprehensive Considerations on Maser Properties of Red Supergiants Associated with Massive Clusters". The Astrophysical Journal. 760: 65. arXiv:1209.6427. doi:10.1088/0004-637X/760/1/65.
  10. ↑ Blum, R. D; Ramirez, Solange V; Sellgren, K; Olsen, K (2003). "Really Cool Stars and the Star Formation History at the Galactic Center". The Astrophysical Journal. 597: 323–346. doi:10.1086/378380.
  11. ↑ Moffat, A. F. J. (August 1976). "Mass loss from the M 3 supergiant HD 143183 in a young compact star cluster in Norma". Astronomy and Astrophysics. 50 (3): 429–434. Bibcode:1976A&A....50..429M.
  12. ↑ Wittkowski, M.; Hauschildt, P. H.; Arroyo-Torres, B.; Marcaide, J. M. (2012). "Fundamental properties and atmospheric structure of the red supergiant VY Canis Majoris based on VLTI/AMBER spectro-interferometry". Astronomy & Astrophysics. 540: L12. arXiv:1203.5194. Bibcode:2012A&A...540L..12W. doi:10.1051/0004-6361/201219126.
  13. ↑ Choi, Yoon Kyung; et al. (2008). "Distance to VY CMa with VERA". Publications of the Astronomical Society of Japan. 60 (5): 1007. arXiv:0808.0641. Bibcode:2008PASJ...60.1007C. doi:10.1093/pasj/60.5.1007.
  14. ↑ Alcolea, J; Bujarrabal, V; Planesas, P; Teyssier, D; Cernicharo, J; De Beck, E; Decin, L; Dominik, C; Justtanont, K; De Koter, A; Marston, A. P; Melnick, G; Menten, K. M; Neufeld, D. A; Olofsson, H; Schmidt, M; Schöier, F. L; Szczerba, R; Waters, L. B. F. M (2013). "HIFISTARSHerschel/HIFI observations of VY Canis Majoris". Astronomy & Astrophysics. 559: A93. doi:10.1051/0004-6361/201321683.
  15. 1 2 3 4 5 6 7 8 9 10 11 12 13 Davies, B.; Figer, D. F.; Law, C. J.; Kudritzki, R. P.; Najarro, F.; Herrero, A.; MacKenty, J. W. (2008). "The Cool Supergiant Population of the Massive Young Star Cluster RSGC1". The Astrophysical Journal. 676 (2): 1016–1028. arXiv:0711.4757. Bibcode:2008ApJ...676.1016D. doi:10.1086/527350.
  16. 1 2 3 4 5 6 7 8 9 10 11 12 Marshall, Jonathan R; van Loon, Jacco Th; Matsuura, Mikako; Wood, Peter R; Zijlstra, Albert A; Whitelock, Patricia A (2004). "The AGB superwind speed at low metallicity". Monthly Notices of the Royal Astronomical Society. 355 (4): 1348. arXiv:astro-ph/0410120. doi:10.1111/j.1365-2966.2004.08417.x.
  17. ↑ Chesneau, O.; Meilland, A.; Chapellier, E.; Millour, F.; Van Genderen, A. M.; Nazé, Y.; Smith, N.; Spang, A.; Smoker, J. V.; Dessart, L.; Kanaan, S.; Bendjoya, Ph.; Feast, M. W.; Groh, J. H.; Lobel, A.; Nardetto, N.; Otero, S.; Oudmaijer, R. D.; Tekola, A. G.; Whitelock, P. A.; Arcos, C.; Curé, M.; Vanzi, L. (2014). "The yellow hypergiant HR 5171 A: Resolving a massive interacting binary in the common envelope phase". Astronomy & Astrophysics. 563: A71. arXiv:1401.2628v2. Bibcode:2014A&A...563A..71C. doi:10.1051/0004-6361/201322421.
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