List of largest stars

Not to be confused with List of most massive stars.

Relative sizes of the planets in the Solar System and some of the largest stars:

Below is a list of the largest stars so far discovered, ordered by radius. The unit of measurement used is the radius of the Sun (695,700 km; 432,288 mi).

Caveats

UY Scuti as seen in visible light.

The exact order of this list is not complete, nor is it perfectly defined:

List

This list is incomplete; you can help by expanding it.
List of the largest stars
Star Solar radii
 (Sun = 1) 		Notes Ref.
UY Scuti 1,708 Margin of error in size determination: ± 192 solar radii. At its smallest, its size would be similar to that of V354 Cephei (see below). [2]
WOH G64 1,635 This would be the largest star in the LMC, but is unusual in position and motion and might still be a foreground halo giant. Margin of possible error: ± 5% solar radii. [3][4]
RW Cephei 1,535 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. [5][6]
Westerlund 1-26 1,530 Very uncertain parameters for an unusual star with strong radio emission. The spectrum is variable but apparently the luminosity is not. [7]
V354 Cephei 1,520 [8]
KY Cygni 1,420–2,850 KY Cygni is located in a region with heavy dust extinction, thus making it hard to determine its size. The quoted size is the value consistent with stellar evolutionary models, the true range may be larger but its value is not known. The value in parentheses is consistent when taken using a higher luminosity value. [8]
VY Canis Majoris 1,420 Humphreys et al originally estimated the radius of VY CMa to be at 1,800–2,100 solar radii; a size so large that places it outside the bounds of stellar evolutionary theory. The quoted size is based on an improved measurement by Wittowski et al In another opinion (such as Massey, Levesque, and Plez's study) say that the star has a radius around 600 solar radii. Margin of possible error: ± 120 solar radii. [9][10]
AH Scorpii 1,411 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. Margin of possible error in size determination: ± 124 solar radii. [2]
VX Sagittarii 1,350–1,940 VX Sgr is a pulsating variable with a large visual range and varies significantly in size. [11]
V766 Centauri A 1,315 Also known as HR 5171 A. V766 Centauri 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. Margin of possible error: ± 260 solar radii. [12]
SMC 18136 1,310 [1]
Mu Cephei 1,260 Also known as Herschel's "Garnet Star". [13]
XX Persei 1,250 Near the bortder with Andromeda.
HV 11423 1,060–1,220 [14]
IRC-10414 1,200 IRC-10414 is a red supergiant companion to WR 114 (a Wolf-Rayet star). [15]
PZ Cassiopeiae 1,190–1,940 PZ Cas is located in a region with heavy dust extinction. The upper estimate is due to an unusual K band measurement and thought to be an artifact of a reddening correction error. The lower estimate is consistent with other stars in the same survey and with theoretical models. In another opinion (such as Kusuno and Oyama) say that the star has a radius around between 1,260–1,340 solar radii. [16][8]
NML Cygni 1,183 NML Cyg is a semiregular variable star surrounded by a circumstellar nebula and is heavily obscured by dust extinction. [17]
EV Carinae 1,168 [18]
RT Carinae 1,090 [8]
V396 Centauri 1,070 [8]
CK Carinae 1,060 [8]
VV Cephei A 1,050 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. Analysis of its orbit places a firm upper limit on the size at 1,900 solar radii. Older estimates have given much larger sizes. [19] [20] [foot 1]
V602 Carinae 1,050 [21]
V1749 Cygni 1,040 [8]
KW Sagittarii 1,009 Margin of possible error : ± 142 solar radii. [2]
NR Vulpeculae 980 [8]
GCIRS 7 960 GCIRS 7 is marginally resolved at H band. We detect a significant circumstellar contribution at K band. The star and its environment are variable in size. Margin of possible error : ± 92 solar radii. [22]
U Lacertae 957
S Cassiopeiae 930 The largest S-type star existent in Milky Way. [23][24]
IX Carinae 920 [8]
BI Cygni 916–1,240 [8][25]
V366 Andromedae 913
Betelgeuse 887 Also known as Alpha Orionis. Ninth brightest star in the night sky. The angular diameter of Betelgeuse is only exceeded by R Doradus and the Sun. Margin of possible error : ± 203 solar radii. [26]
Antares A 883 [27]
BC Cygni 856–1,553 [28]
V384 Puppis 850 [8]
Theta Muscae Ac 804 Although it is the lightest star in the Theta Muscae system, it is ironically the largest star.
BO Carinae 790 [8]
S Persei 780–1,230 In the Perseus Double Cluster. [8]
SU Persei 780 In the Perseus Double Cluster [8]
V355 Cephei 770 [8]
S Cephei 760 The largest carbon star star existent in Milky Way.
RS Persei 740–800 In the Perseus Double Cluster. [29]
V648 Cassiopeiae 710 [8]
V382 Carinae 700 Yellow hypergiant, one of the rarest types of star. [30]
CW Leonis 700 [31]
V528 Carinae 700 [8]
The following well-known stars are listed for the purpose of comparison.
Star name Solar radii
(Sun = 1)		 Notes Ref.
V509 Cassiopeiae 650 Yellow hypergiant, one of the rarest types of a star. [32]
Rho Cassiopeiae 450 Yellow hypergiant, one of the rarest types of a star. [33]
Eta Carinae A 430 Also known as Tseen She. 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. [34]
R Leporis 400 Also known as Hind's "Crimson Star". One of the largest carbon stars existent in the Milky Way. Margin of possible error : ± 90 solar radii. [35]
La Superba 390 Also known as Y Canum Venaticorum. Currently one of the coolest and reddest stars. [36]
V838 Monocerotis 380 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. Margin of possible error : ± 90 solar radii. [37]
S Doradus 100–380 Prototype S Doradus variable. [38]
R Doradus 370 Star with the second largest apparent size after the Sun. Margin of possible error : ± 50 solar radii. [39]
Mira A 367 Also known as Omicron Ceti. Prototype Mira variable. [40]
The Pistol Star 306 Blue hypergiant, currently among the most massive and luminous stars. [41]
Alpha Herculis A 264–303 Also known as Ras Algethi. [42]
Deneb 220 Also known as Alpha Cygni. 19th brightest star in the night sky. Margin of possible error : ± 17 solar radii. [43]
Peony Nebula Star 92 Candidate for most luminous star in the Milky Way. [44]
Rigel 78.9 Also known as Beta Orionis. Seventh brightest star in the night sky. Margin of possible error : ± 7.4 solar radii. [45]
Canopus 71 Also known as Alpha Carinae. Second brightest star in the night sky. Margin of possible error : ± 7 solar radii. [46]
Aldebaran 44.2 Also known as Alpha Tauri. [47]
R136a1 35.4 Also on the list as the most massive and luminous star. [48]
HDE 226868 20–22 The supergiant companion of black hole Cygnus X-1. The black hole is 500,000 times smaller than the star. [49]

See also

Footnotes

  1. ↑ Size, mass and luminosity estimates of the VV Cephei system are all considerably uncertain due to insufficient knowledge: Professor Kaler writes "in truth we really do not know". Its distance cannot be measured from parallax, instead it is derived from its assumed membership in the Cepheus OB2 association, but this is also not certain. Other methods give a range of sizes between 1,000 and 2,200 that of the Sun, but these too are confounded by the fact that the star is not spherical, which leads to overestimates. (J. Kaler)

References

  1. 1 2 Levesque, E. M.; Massey, P.; Olsen, K. A. G.; Plez, B.; Meynet, G.; Maeder, A. (2006). "The Effective Temperatures and Physical Properties of Magellanic Cloud Red Supergiants: The Effects of Metallicity". The Astrophysical Journal. 645 (2): 1102. arXiv:astro-ph/0603596Freely accessible. Bibcode:2006ApJ...645.1102L. doi:10.1086/504417.
  2. 1 2 3 Arroyo-Torres, B.; Wittkowski, M.; Marcaide, J. M.; Hauschildt, P. H. (2013). "The atmospheric structure and fundamental parameters of the red supergiants AH Scorpii, UY Scuti, and KW Sagittarii". Astronomy & Astrophysics. 554: A76. arXiv:1305.6179Freely accessible. Bibcode:2013A&A...554A..76A. doi:10.1051/0004-6361/201220920.
  3. ↑ Emily M. Levesque; Philip Massey; Bertrand Plez & Knut A. G. Olsen (June 2009). "The Physical Properties of the Red Supergiant WOH G64: The Largest Star Known?". Astronomical Journal. 137 (6): 4744. arXiv:0903.2260Freely accessible. Bibcode:2009AJ....137.4744L. doi:10.1088/0004-6256/137/6/4744.
  4. ↑ 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.
  5. ↑ 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.
  6. ↑ 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:1005.1008Freely accessible. Bibcode:2010MNRAS.407.1203D. doi:10.1111/j.1365-2966.2010.16965.x.
  7. ↑ Wright, N. J.; Wesson, R.; Drew, J. E.; Barentsen, G.; Barlow, M. J.; Walsh, J. R.; Zijlstra, A.; Drake, J. J.; Eisloffel, J.; Farnhill, H. J. (16 October 2013). "The ionized nebula surrounding the red supergiant W26 in Westerlund 1". Monthly Notices of the Royal Astronomical Society: Letters. 437 (1): L1–L5. arXiv:1309.4086Freely accessible. Bibcode:2014MNRAS.437L...1W. doi:10.1093/mnrasl/slt127.
  8. 1 2 3 4 5 6 7 8 9 10 11 12 13 14 15 16 17 Levesque, E. M.; Massey, P.; Olsen, K. A. G.; Plez, B.; Josselin, E.; Maeder, A.; Meynet, G. (2005). "The Effective Temperature Scale of Galactic Red Supergiants: Cool, but Not as Cool as We Thought". The Astrophysical Journal. 628 (2): 973. arXiv:astro-ph/0504337Freely accessible. Bibcode:2005ApJ...628..973L. doi:10.1086/430901.
  9. ↑ 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:1203.5194Freely accessible. Bibcode:2012A&A...540L..12W. doi:10.1051/0004-6361/201219126.
  10. ↑ Choi, Yoon Kyung; Hirota, Tomoya; Honma, Mareki; Kobayashi, Hideyuki; Bushimata, Takeshi; Imai, Hiroshi; Iwadate, Kenzaburo; Jike, Takaaki; Kameno, Seiji; Kameya, Osamu; Kamohara, Ryuichi; Kan-Ya, Yukitoshi; Kawaguchi, Noriyuki; Kijima, Masachika; Kim, Mi Kyoung; Kuji, Seisuke; Kurayama, Tomoharu; Manabe, Seiji; Maruyama, Kenta; Matsui, Makoto; Matsumoto, Naoko; Miyaji, Takeshi; Nagayama, Takumi; Nakagawa, Akiharu; Nakamura, Kayoko; Oh, Chung Sik; Omodaka, Toshihiro; Oyama, Tomoaki; Sakai, Satoshi; et al. (2008). "Distance to VY CMa with VERA". Publications of the Astronomical Society of Japan. Publications Astronomical Society of Japan. 60 (5): 1007. arXiv:0808.0641Freely accessible. Bibcode:2008PASJ...60.1007C. doi:10.1093/pasj/60.5.1007.
  11. ↑ Lockwood, G.W.; Wing, R. F. (1982). "The light and spectrum variations of VX Sagittarii, an extremely cool supergiant". Monthly Notices of the Royal Astronomical Society. 198 (2): 385–404. Bibcode:1982MNRAS.198..385L. doi:10.1093/mnras/198.2.385.
  12. ↑ o. Chesneau; a. Meilland; e. Chapellier; f. Millour; a.m. Van Genderen; y. Naze; n. Smith; a. Spang; et al. (2014). "The yellow hypergiant HR 5171 A: Resolving a massive interacting binary in the common envelope phase". Astronomy & Astrophysics. 563: A71. arXiv:1401.2628Freely accessible. Bibcode:2014A&A...563A..71C. doi:10.1051/0004-6361/201322421.
  13. ↑ Josselin, E.; Plez, B. (2007). "Atmospheric dynamics and the mass loss process in red supergiant stars". Astronomy and Astrophysics. 469 (2): 671–680. arXiv:0705.0266Freely accessible. Bibcode:2007A&A...469..671J. doi:10.1051/0004-6361:20066353.
  14. ↑ Massey, Philip; Levesque, Emily M.; Olsen, K. A. G.; Plez, Bertrand; Skiff, B. A. (2007). "HV 11423: The Coolest Supergiant in the SMC". The Astrophysical Journal. 660: 301. arXiv:astro-ph/0701769Freely accessible. Bibcode:2007ApJ...660..301M. doi:10.1086/513182.
  15. ↑ Gvaramadze, V. V.; Menten, K. M.; Kniazev, A. Y.; Langer, N.; MacKey, J.; Kraus, A.; Meyer, D. M.-A.; Kamiński, T. (2014). "IRC -10414: A bow-shock-producing red supergiant star". Monthly Notices of the Royal Astronomical Society. 437: 843. arXiv:1310.2245Freely accessible. Bibcode:2014MNRAS.437..843G. doi:10.1093/mnras/stt1943.
  16. ↑ Kusuno, K.; Asaki, Y.; Imai, H.; Oyama, T. (2013). "Distance and Proper Motion Measurement of the Red Supergiant, Pz Cas, in Very Long Baseline Interferometry H2O Maser Astrometry". The Astrophysical Journal. 774 (2): 107. arXiv:1308.3580Freely accessible. Bibcode:2013ApJ...774..107K. doi:10.1088/0004-637X/774/2/107.
  17. ↑ De Beck, E.; Decin, L.; De Koter, A.; Justtanont, K.; Verhoelst, T.; Kemper, F.; Menten, K. M. (2010). "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". Astronomy and Astrophysics. 523: A18. arXiv:1008.1083Freely accessible. Bibcode:2010A&A...523A..18D. doi:10.1051/0004-6361/200913771.
  18. ↑ Van Loon, J. Th.; Cioni, M.-R. L.; Zijlstra, A. A.; Loup, C. (2005). "An empirical formula for the mass-loss rates of dust-enshrouded red supergiants and oxygen-rich Asymptotic Giant Branch stars". Astronomy and Astrophysics. 438: 273. arXiv:astro-ph/0504379Freely accessible. Bibcode:2005A&A...438..273V. doi:10.1051/0004-6361:20042555.
  19. ↑ Bauer, W. H.; Gull, T. R.; Bennett, P. D. (2008). "Spatial Extension in the Ultraviolet Spectrum of Vv Cephei". The Astronomical Journal. 136 (3): 1312. Bibcode:2008AJ....136.1312H. doi:10.1088/0004-6256/136/3/1312.
  20. ↑ Professor James B. (Jim) Kaler. "VV CEP (VV Cephei)". University of Illinois. Retrieved 2010-03-15.
  21. ↑ Arroyo-Torres, B.; Wittkowski, M.; Chiavassa, A.; Scholz, M.; Freytag, B.; Marcaide, J. M.; Hauschildt, P. H.; Wood, P. R.; Abellan, F. J. (2015). "What causes the large extensions of red supergiant atmospheres?. Comparisons of interferometric observations with 1D hydrostatic, 3D convection, and 1D pulsating model atmospheres". Astronomy & Astrophysics. 575: A50. arXiv:1501.01560Freely accessible. Bibcode:2015A&A...575A..50A. doi:10.1051/0004-6361/201425212.
  22. ↑ Paumard, T.; Pfuhl, O.; Martins, F.; Kervella, P.; Ott, T.; Pott, J.-U.; Le Bouquin, J. B.; Breitfelder, J.; Gillessen, S.; Perrin, G.; Burtscher, L.; Haubois, X.; Brandner, W. (2014). "GCIRS 7, a pulsating M1 supergiant at the Galactic centre. Physical properties and age". Astronomy & Astrophysics. 568 (85): A85. arXiv:1406.5320Freely accessible. Bibcode:2014A&A...568A..85P. doi:10.1051/0004-6361/201423991.
  23. ↑ Ramstedt, S.; Schöier, F. L.; Olofsson, H. (2009). "Circumstellar molecular line emission from S-type AGB stars: mass-loss rates and SiO abundances". Astronomy and Astrophysics. 499 (2). Bibcode:2009A&A...499..515R. 515-527.
  24. ↑ Ramstedt, S.; Schöier, F. L.; Olofsson, H.; Lundgren, A. A. (2006). "Mass-loss properties of S-stars on the AGB". Astronomy and Astrophysics. 454 (2): L103. Bibcode:2006A&A...454L.103R. doi:10.1051/0004-6361:20065285.
  25. ↑ Mauron, N.; Josselin, E. (2011). "The mass-loss rates of red supergiants and the de Jager prescription". Astronomy and Astrophysics. 526: A156. arXiv:1010.5369Freely accessible. Bibcode:2011A&A...526A.156M. doi:10.1051/0004-6361/201013993.
  26. ↑ Smith, Nathan; Hinkle, Kenneth H.; Ryde, Nils (March 2009). "Red Supergiants as Potential Type IIn Supernova Progenitors: Spatially Resolved 4.6 μm CO Emission Around VY CMa and Betelgeuse". The Astronomical Journal. 137 (3): 3558–3573. arXiv:0811.3037Freely accessible. Bibcode:2009AJ....137.3558S. doi:10.1088/0004-6256/137/3/3558.
  27. ↑ Baade, R.; Reimers, D. (October 2007). "Multi-component absorption lines in the HST spectra of α Scorpii B". Astronomy and Astrophysics. 474 (1): 229–237. Bibcode:2007A&A...474..229B. doi:10.1051/0004-6361:20077308.
  28. ↑ Turner, David G.; Rohanizadegan, Mina; Berdnikov, Leonid N.; Pastukhova, Elena N. (2006). "The Long-Term Behavior of the Semiregular M Supergiant Variable BC Cygni". The Publications of the Astronomical Society of the Pacific. 118 (849): 1533. Bibcode:2006PASP..118.1533T. doi:10.1086/508905.
  29. ↑ Baron, F.; Monnier, J. D.; Kiss, L. L.; Neilson, H. R.; Zhao, M.; Anderson, M.; Aarnio, A.; Pedretti, E.; Thureau, N.; Ten Brummelaar, T. A.; Ridgway, S. T.; McAlister, H. A.; Sturmann, J.; Sturmann, L.; Turner, N. (2014). "CHARA/MIRC Observations of Two M Supergiants in Perseus OB1: Temperature, Bayesian Modeling, and Compressed Sensing Imaging". The Astrophysical Journal. 785: 46. arXiv:1405.4032Freely accessible. Bibcode:2014ApJ...785...46B. doi:10.1088/0004-637X/785/1/46.
  30. ↑ Achmad, L.; et al. (1992). "A photometric study of the G0-4 Ia(+) hypergiant HD 96918 (V382 Carinae)". Astronomy and Astrophysics. 259: 600–606. Bibcode:1992A&A...259..600A.
  31. ↑ Weigelt, G.; et al. (May 1998), "76mas speckle-masking interferometry of IRC+10216 with the SAO 6m telescope: Evidence for a clumpy shell structure", Astronomy and Astrophysics, 333: L51–L54, arXiv:astro-ph/9805022Freely accessible, Bibcode:1998A&A...333L..51W
  32. ↑ Nieuwenhuijzen, H.; De Jager, C.; Kolka, I.; Israelian, G.; Lobel, A.; Zsoldos, E.; Maeder, A.; Meynet, G. (2012). "The hypergiant HR 8752 evolving through the yellow evolutionary void". Astronomy & Astrophysics. 546: A105. Bibcode:2012A&A...546A.105N. doi:10.1051/0004-6361/201117166.
  33. ↑ Gorlova, N.; Lobel, A.; Burgasser, A. J.; Rieke, G. H.; Ilyin, I.; Stauffer, J. R. (2006). "On the CO Near‐Infrared Band and the Line‐splitting Phenomenon in the Yellow Hypergiant ρ Cassiopeiae". The Astrophysical Journal. 651 (2): 1130–1150. arXiv:astro-ph/0607158Freely accessible. Bibcode:2006ApJ...651.1130G. doi:10.1086/507590.
  34. ↑ Gull, T. R.; Damineli, A. (2010). "JD13 – Eta Carinae in the Context of the Most Massive Stars". Proceedings of the International Astronomical Union. 5: 373. arXiv:0910.3158Freely accessible. Bibcode:2010HiA....15..373G. doi:10.1017/S1743921310009890.
  35. ↑ Hofmann, K.-H.; Eberhardt, M.; Driebe, T.; Schertl, D.; Scholz, M.; Schoeller, M.; Weigelt, G.; Wittkowski, M.; Woodruff, H. C. (2005). "Interferometric observations of the Mira star o Ceti with the VLTI/VINCI instrument in the near-infrared". Proceedings of the 13th Cambridge Workshop on Cool Stars. 560: 651. Bibcode:2005ESASP.560..651H.
  36. ↑ Luttermoser, Donald G.; Brown, Alexander (1992). "A VLA 3.6 centimeter survey of N-type carbon stars". Astrophysical Journal. 384: 634. Bibcode:1992ApJ...384..634L. doi:10.1086/170905.
  37. ↑ Tylenda, R.; Kamiński, T.; Schmidt, M.; Kurtev, R.; Tomov, T. (2011). "High-resolution optical spectroscopy of V838 Monocerotis in 2009". Astronomy & Astrophysics. 532: A138. arXiv:1103.1763Freely accessible. Bibcode:2011A&A...532A.138T. doi:10.1051/0004-6361/201116858.
  38. ↑ Lamers, H. J. G. L. M. (February 6–10, 1995). "Observations and Interpretation of Luminous Blue Variables". Proceedings of IAU Colloquium 155, Astrophysical applications of stellar pulsation. Astrophysical applications of stellar pulsation. Astronomical Society of the Pacific Conference Series. 83. Cape Town, South Africa: Astronomical Society of the Pacific. pp. 176–191. Bibcode:1995ASPC...83..176L.
  39. ↑ Bedding, T. R.; et al. (April 1997), "The angular diameter of R Doradus: a nearby Mira-like star", Monthly Notices of the Royal Astronomical Society, 286 (4): 957–962, arXiv:astro-ph/9701021Freely accessible, Bibcode:1997MNRAS.286..957B, doi:10.1093/mnras/286.4.957
  40. ↑ Woodruff, H. C.; Eberhardt, M.; Driebe, T.; Hofmann, K.-H.; et al. (2004). "Interferometric observations of the Mira star o Ceti with the VLTI/VINCI instrument in the near-infrared". Astronomy & Astrophysics. 421 (2): 703–714. arXiv:astro-ph/0404248Freely accessible. Bibcode:2004A&A...421..703W. doi:10.1051/0004-6361:20035826.
  41. ↑ Najarro, F.; Figer, D. F.; Hillier, D. J.; Geballe, T. R.; Kudritzki, R. P. (2009). "Metallicity in the Galactic Center: The Quintuplet Cluster". The Astrophysical Journal. 691 (2): 1816. arXiv:0809.3185Freely accessible. Bibcode:2009ApJ...691.1816N. doi:10.1088/0004-637X/691/2/1816.
  42. ↑ Moravveji, Ehsan; Guinan, Edward F.; Khosroshahi, Habib; Wasatonic, Rick (2013). "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". The Astronomical Journal. 146 (6): 148. arXiv:1308.1632Freely accessible. Bibcode:2013AJ....146..148M. doi:10.1088/0004-6256/146/6/148.
  43. ↑ Schiller, F.; Przybilla, N. (2008). "Quantitative spectroscopy of Deneb". Astronomy & Astrophysics. 479 (3): 849–858. arXiv:0712.0040Freely accessible. Bibcode:2008A&A...479..849S. doi:10.1051/0004-6361:20078590.
  44. ↑ Barniske, A.; Oskinova, L. M.; Hamann, W. -R. (2008). "Two extremely luminous WN stars in the Galactic center with circumstellar emission from dust and gas". Astronomy and Astrophysics. 486 (3): 971. arXiv:0807.2476Freely accessible. Bibcode:2008A&A...486..971B. doi:10.1051/0004-6361:200809568.
  45. ↑ Moravveji, Ehsan; Guinan, Edward F.; Shultz, Matt; Williamson, Michael H.; Moya, Andres (March 2012). "Asteroseismology of the nearby SN-II Progenitor: Rigel. Part I. The MOST High-precision Photometry and Radial Velocity Monitoring". The Astrophysical Journal. 747 (1): 108–115. arXiv:1201.0843Freely accessible. Bibcode:2012ApJ...747..108M. doi:10.1088/0004-637X/747/2/108.
  46. ↑ Cruzalèbes, P.; Jorissen, A.; Rabbia, Y.; Sacuto, S.; Chiavassa, A.; Pasquato, E.; Plez, B.; Eriksson, K.; Spang, A.; Chesneau, O. (2013). "Fundamental parameters of 16 late-type stars derived from their angular diameter measured with VLTI/AMBER". Monthly Notices of the Royal Astronomical Society. 434: 437. arXiv:1306.3288Freely accessible. Bibcode:2013MNRAS.434..437C. doi:10.1093/mnras/stt1037.
  47. ↑ Richichi, A.; Roccatagliata, V. (2005). "Aldebaran's angular diameter: how well do we know it?". Astronomy and Astrophysics. 433: 305–312. arXiv:astro-ph/0502181Freely accessible. Bibcode:2005A&A...433..305R. doi:10.1051/0004-6361:20041765.
  48. ↑ Crowther, P. A.; Schnurr, O.; Hirschi, R.; Yusof, N.; Parker, R. J.; Goodwin, S. P.; Kassim, H. A. (2010). "The R136 star cluster hosts several stars whose individual masses greatly exceed the accepted 150 M⊙ stellar mass limit". Monthly Notices of the Royal Astronomical Society. 408 (2): 731. arXiv:1007.3284Freely accessible. Bibcode:2010MNRAS.408..731C. doi:10.1111/j.1365-2966.2010.17167.x.
  49. ↑ Ziółkowski, J. (2005), "Evolutionary constraints on the masses of the components of HDE 226868/Cyg X-1 binary system", Monthly Notices of the Royal Astronomical Society, 358 (3): 851–859, arXiv:astro-ph/0501102Freely accessible, Bibcode:2005MNRAS.358..851Z, doi:10.1111/j.1365-2966.2005.08796.x Note: for radius and luminosity, see Table 1 with d=2 kpc.

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