Usuario:JoeyPknowsalotaboutthat/Taller

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List[editar]

List of the largest stars
Star name Solar radii
(Sun = 1) 		Notes
Red giants of Westerlund 1 2,000[1]​ Not yet properly identified, and currently cannot be hailed as the largest known star.
UY Scuti 1,708 ± 192[2]​ Currently the largest star in the Milky Way and in the universe. Margin of error in size determination: ±192 solar radii. At the smallest, it would have a size similar to VX Sagittarii (see below)
WOH G64 1,540 ± 77[3]​ This would be the largest star in the LMC, but is unusual in position and motion and might still be a foreground halo giant. Ohnaka (2009) calculates 2,000 R☉.[4]​
RW Cephei 1,535 [5]​[6]​ 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 sizes are just estimates.
Westerlund 1-26 1,530[7]​–2,544[1]​ Very uncertain parameters for an unusual star with strong radio emission. The spectrum is variable but apparently the luminosity is not. The largest value given was once listed in an earlier version of the reference, but was later removed due to lack of references, and is subject to inaccuracy and not perfectly defined.
VX Sagittarii 1,520[8]​ VX Sgr is a pulsating variable with a large visual range from 1,350 R☉ to 1,940 R☉ and varies significantly in size.[9]​
KY Cygni 1,420–2,850 [10]​ The 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.
VY Canis Majoris 1,420 ± 120[11]​ Once thought to be a star so large that it contradicted stellar evolutionary theory with a radius of 1,800 R☉ to 2,200 R☉,[12]​ improved measurements have brought it down to size.[11]​[13]​
AH Scorpii 1,411 ± 124[2]​ 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 A 1,400[14]​ or 1,050–1,800[15]​ 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. Older estimates have given much larger sizes.[16]​
HR 5171 A 1,315 ± 260 HR 5171 A is a highly distorted star in a close binary system, losing mass to the secondary. It is the largest known yellow star. Its size can be calculated from its angular diameter, which has been measured using the AMBER instrument and VLTI.
SMC 018136 1,310[17]​ This would be the largest star in the SMC.
Mu Cephei (Herschel's "Garnet Star") 1,260[18]​ or 650[19]​–1,420[10]​ The reddest star in the night sky.
BI Cygni 1,240[10]​
S Persei 1,230[10]​ In the Perseus Double Cluster.
RAFGL 2139 1,200[20]​ RAFGL 2139 is a rare red supergiant companion to WR 114 that has a bow shock.
PZ Cassiopeiae 1,190-1,940[10]​ or 1,260-1,340[21]​ The largest estimate is due to an unusual K band measurement and thought to be an artifact of a reddening correction error. The lowest 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.
NML Cygni 1,183[22]​–2,770 or 1,640[23]​ An accurate measure of its distance and its luminosity combined with assumptions of its temperature give 1,640 R☉ for 3,250 K or 2,770 R☉ for 2,500 K.
EV Carinae 1,168[24]​-2,880[25]​ EV Car is an unstable star plagued by dust extinction. The value on the left is subject to inaccuracy and thus not yet well defined.
BC Cygni 1,140[10]​-1,230[18]​ Other recent estimates range from 856 R☉ to 1,553 R☉.[26]​
RT Carinae 1,090[10]​
V396 Centauri 1,070[10]​
HV 11423 1,060–1,220[27]​ HV 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 Carinae 1,060[10]​
U Lacertae 1,025[8]​
KW Sagittarii 1,009[2]​-1,460[10]​ Margin of possible error: ± 142 solar radii (Torres 2013).
NR Vulpeculae 980[10]​
GCIRS 7 960±92[28]​
S Cassiopeiae 930[29]​[30]​
IX Carinae 920[10]​
HV 2112 918[31]​ Most likely candidate for a Thorne-Zytkow Object.
NSV 25875 891[22]​
Betelgeuse (Alpha Orionis) 887[32]​–1,200[33]​ Margin of possible error: ±203 solar radii (Dolan 2016) or ±217 solar radii (Neilson 2011). At the largest, it would have a size similar to Jupiter's orbit
V437 Scuti 874[22]​
V602 Carinae 860[10]​-1,050[34]​ Margin of possible error: ± 165 solar radii (Torres 2015).
V669 Cassiopeiae 859[22]​
V1185 Scorpii 830[22]​
Antares A (Alpha Scorpii A) 800–900[35]​ 15th brightest star in the Night Sky. Ohnaka (2013) calculates 680 R☉.[36]​
BO Carinae 790[10]​
SU Persei 780[10]​ In the Perseus Double Cluster
RS Persei 770[37]​-1,000[10]​ In the Perseus Double Cluster. Margin of possible error: ± 30 solar radii (Baron 2014).
AV Persei 770[10]​ In the Perseus Double Cluster
V355 Cepheus 300[8]​-770[10]​
V915 Scorpii 760[38]​
S Cephei 760[39]​
HD 303250 750[10]​
V382 Carinae 747[40]​ The brightest yellow hypergiant in the night sky, one of the rarest types of star. Achmad (1992) calculates 700 ± 250 R☉.[41]​
RU Virginis 742[39]​
XX Persei 710[42]​ In the Perseus Double Cluster
V528 Carinae 700[10]​
V354 Cephei 690[8]​-1,520[10]​
TV Geminorum 620-710[10]​
CE Tauri ("Ruby Star")[43]​ 608[44]​ Can be occulted by the Moon, allowing accurate determination of its apparent diameter.
S Pegasi 459–574[45]​
T Cephei 540[46]​
S Orionis 530[47]​ A pulsating Mira variable.
W Hydrae 520[48]​
R Leporis (Hind's "Crimson Star") 500[cita requerida] or 400–535[49]​ One of the largest carbon stars existent in the Milky Way. Margin of possible error: ± 90 solar radii.
The following well-known stars are listed for the purpose of comparison.
Rho Cassiopeiae 400-500[50]​ Yellow hypergiant, one of the rarest types of a star.
Mira A (Omicron Ceti) 332–402[51]​ Prototype Mira variable. De beck (2005) calculates 541 R☉.[22]​
V509 Cassiopeiae 400–900[52]​ Yellow hypergiant, one of the rarest types of a star.
V838 Monocerotis 380 (in 2009)[53]​ A short time after the outburst V838 Mon was measured at 1,570 ± 400 R☉.[54]​ However the distance to this "L 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.
S Doradus 100-380[55]​ Prototype S Doradus variable
R Doradus 370[56]​ Star with the second largest apparent size after the Sun.
The Pistol Star 340[57]​ Blue hypergiant, among the most massive and luminous stars known.
La Superba (Y Canum Venaticorum) 300[22]​ Currently one of the coolest and reddest stars.
Alpha Herculis (Ras Algethi) 284 ± 60[58]​ Moravveji et al also gives a range from 264 R☉ to 303 R☉. At an estimated distance of 110 parsecs from the Sun, this corresponds to a radius of 400 ± 61 R☉.[58]​
Sun's red giant phase 256[59]​
 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. (see below)
Reported for reference
Eta Carinae A (Tseen She) 250[60]​ 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. one study calculated 60 R☉, but at optical depth 0.67, the size would be 800 R☉.[61]​ At the peak of the Great Eruption, it would have a size similar to VV Cephei A.[62]​ Other recent estimates range from 85 R☉ to 195 R☉.[63]​
CW Leonis 250–500[64]​ CW Leonis has been one of the mistaken identities as the claimed planet "Nibiru" or "Planet X", due to its brightness as it approaches 1st magnitude. Other recent estimates range from 700 R☉[65]​ to 826 R☉[22]​.
Orbit of Earth 211 - 219 Reported for reference
Deneb (Alpha Cygni) 203[66]​
LBV 1806-20 200[67]​ Formerly a candidate for the most luminous star in the Milky Way.
Epsilon Aurigae A (Almaaz) 143-358[68]​ ε Aur was incorrectly hailed as the largest star with a radius 2,000 R☉ or 3,000 R☉,[69]​ even though it later turned out not to be an infrared light star but rather a dusk torus surrounding the system.
Peony Nebula Star 92-100[70]​ Candidate for most luminous star in the Milky Way.
Rigel A (Beta Orionis A) 78.9[71]​
Canopus (Alpha Carinae) 71[72]​ Second brightest star in the night sky.
Albireo A 69 Popular example of a binary star.
Aldebaran (Alpha Tauri) 44.2[73]​
Polaris (Alpha Ursae Minoris) 37.5[74]​ The current northern pole star.
R136a1 35.4[75]​ Also on record as the most massive and luminous star known.
Arcturus (Alpha Boötis) 25.4[76]​ Brightest star in the northern hemisphere.
HDE 226868 20-22[77]​ The supergiant companion of black hole Cygnus X-1. The black hole is 500,000 times smaller than the star.
VV Cephei B 13[16]​-25[78]​ The B-type main sequence companion of VV Cephei A.
Capella A (Alpha Aurigae A) 11.98 6th brightest star in the night sky.
WR 104 10 Located 8,000 light years away from us, this star could destroy life on Earth with its self-destructive frenzy.
Sun 1 The largest object in the Solar System.
Reported for reference

References[editar]

  1. ↑ a b Clark, J. S.; Ritchie, B. W.; Negueruela, I.; Crowther, P. A.; Damineli, A.; Jablonski, F. J.; Langer, N. (2011). «A VLT/FLAMES survey for massive binaries in Westerlund 1. III. The WC9d binary W239 and implications for massive stellar evolution». Astronomy & Astrophysics 531: A28. Bibcode:2011A&A...531A..28C. arXiv:1105.0776. doi:10.1051/0004-6361/201116990. 
  2. ↑ a b c 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. Bibcode:2013A&A...554A..76A. arXiv:1305.6179. doi:10.1051/0004-6361/201220920. 
  3. ↑ 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. Bibcode:2009AJ....137.4744L. arXiv:0903.2260. 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. 
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  8. ↑ a b c d Mauron, N.; Josselin, E. (2011). «The mass-loss rates of red supergiants and the de Jager prescription». Astronomy and Astrophysics 526: A156. Bibcode:2011A&A...526A.156M. arXiv:1010.5369. doi:10.1051/0004-6361/201013993. 
  9. ↑ 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. 
  10. ↑ a b c d e f g h i j k l m n ñ o p q r s t u 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. Bibcode:2005ApJ...628..973L. arXiv:astro-ph/0504337. doi:10.1086/430901. 
  11. ↑ a b 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. Bibcode:2012A&A...540L..12W. arXiv:1203.5194. doi:10.1051/0004-6361/201219126. 
  12. ↑ Humphreys, Roberta M. (2006). VY Canis Majoris: The Astrophysical Basis of Its Luminosity. pp. arXiv:astro-ph/0610433. Bibcode:2006astro.ph.10433H. arXiv:astro-ph/0610433. 
  13. ↑ Choi, Yoon Kyung et al. (2008). «Distance to VY CMa with VERA». Publications of the Astronomical Society of Japan (Publications Astronomical Society of Japan) 60 (5): 1007. Bibcode:2008PASJ...60.1007C. arXiv:0808.0641. doi:10.1093/pasj/60.5.1007. 
  14. ↑ Ridpath y Tirion, 2001, pp. 112–113.
  15. ↑ 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. 
  16. ↑ a b Wright, K. O. (1977). «The system of VV Cephei derived from an analysis of the H-alpha line». Journal of the Royal Astronomical Society of Canada 71: 152. Bibcode:1977JRASC..71..152W. 
  17. ↑ Error en la cita: Etiqueta <ref> no válida; no se ha definido el contenido de las referencias llamadas mc
  18. ↑ a b Josselin, E.; Plez, B. (2007). «Atmospheric dynamics and the mass loss process in red supergiant stars». Astronomy and Astrophysics 469 (2): 671-680. Bibcode:2007A&A...469..671J. arXiv:0705.0266. doi:10.1051/0004-6361:20066353. 
  19. ↑ Tsuji, Takashi (2000). «Water in Emission in the Infrared Space Observatory Spectrum of the Early M Supergiant Star μ Cephei». The Astrophysical Journal Letters 540 (2): 99-102. Bibcode:2000ApJ...540L..99T. arXiv:astro-ph/0008058. doi:10.1086/312879. 
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  21. ↑ 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. Bibcode:2013ApJ...774..107K. arXiv:1308.3580. doi:10.1088/0004-637X/774/2/107. 
  22. ↑ a b c d e f g h 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. Bibcode:2010A&A...523A..18D. arXiv:1008.1083. doi:10.1051/0004-6361/200913771. 
  23. ↑ Zhang, B.; Reid, M. J.; Menten, K. M.; Zheng, X. W.; Brunthaler, A. (2012). «The distance and size of the red hypergiant NML Cygni from VLBA and VLA astrometry». Astronomy & Astrophysics 544: A42. Bibcode:2012A&A...544A..42Z. arXiv:1207.1850. doi:10.1051/0004-6361/201219587. 
  24. ↑ 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. Bibcode:2005A&A...438..273V. arXiv:astro-ph/0504379. doi:10.1051/0004-6361:20042555. 
  25. ↑ De Jager, C; Nieuwenhuijzen, H; Van Der Hucht, K. A (1988). «Mass loss rates in the Hertzsprung-Russell diagram». Astronomy and Astrophysics Supplement Series (ISSN 0365-0138) 72: 259. Bibcode:1988A&AS...72..259D. 
  26. ↑ 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. 
  27. ↑ 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. Bibcode:2007ApJ...660..301M. arXiv:astro-ph/0701769. doi:10.1086/513182. 
  28. ↑ 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: A85. Bibcode:2014A&A...568A..85P. arXiv:1406.5320. doi:10.1051/0004-6361/201423991. 
  29. ↑ 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): 515-527. Bibcode:2009A&A...499..515R. arXiv:0903.1672. doi:10.1051/0004-6361/200911730. 
  30. ↑ 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. arXiv:astro-ph/0605664. doi:10.1051/0004-6361:20065285. 
  31. ↑ Levesque, Emily M.; Massey, P.; Zytkow, A. N.; Morrell, N. (1 September 2014). «Discovery of a Thorne-̇Żytkow object candidate in the Small Magellanic Cloud». Monthly Notices of the Royal Astronomical Society: Letters 443: L94. Bibcode:2014MNRAS.443L..94L. arXiv:1406.0001. doi:10.1093/mnrasl/slu080. 
  32. ↑ Dolan, Michelle M.; Mathews, Grant J.; Lam, Doan Duc; Lan, Nguyen Quynh; Herczeg, Gregory J.; Dearborn, David S. P. (2016). «Evolutionary Tracks for Betelgeuse». The Astrophysical Journal 819: 7. Bibcode:2016ApJ...819....7D. arXiv:1406.3143v2. doi:10.3847/0004-637X/819/1/7. 
  33. ↑ Neilson, H. R.; Lester, J. B.; Haubois, X. (December 2011). «Weighing Betelgeuse: Measuring the Mass of α Orionis from Stellar Limb-darkening». Astronomical Society of the Pacific. 9th Pacific Rim Conference on Stellar Astrophysics. Proceedings of a conference held at Lijiang, China in 14–20 April 2011. ASP Conference Series, Vol. 451: 117. Bibcode:2010ASPC..425..103L. arXiv:1109.4562. 
  34. ↑ Arroyo-Torres, B.; Wittkowski, M.; Chiavassa, A.; Scholz, M.; Freytag, B.; Marcaide, J. M.; Hauschildt, P. H.; Wood, P. R. et al. (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. Bibcode:2015A&A...575A..50A. arXiv:1501.01560. doi:10.1051/0004-6361/201425212. 
  35. ↑ "Antares: Betelgeuse's Neglected Twin" Aavso.org.
  36. ↑ Ohnaka, K; Hofmann, K.-H; Schertl, D; Weigelt, G; Baffa, C; Chelli, A; Petrov, R; Robbe-Dubois, S (2013). «High spectral resolution imaging of the dynamical atmosphere of the red supergiant Antares in the CO first overtone lines with VLTI/AMBER». Astronomy & Astrophysics 555: A24. Bibcode:2013A&A...555A..24O. arXiv:1304.4800. doi:10.1051/0004-6361/201321063. 
  37. ↑ 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. Bibcode:2014ApJ...785...46B. arXiv:1405.4032. doi:10.1088/0004-637X/785/1/46. 
  38. ↑ Stickland, D. J. (1985). «IRAS observations of the cool galactic hypergiants». The Observatory 105: 229. Bibcode:1985Obs...105..229S. 
  39. ↑ a b Bergeat, J.; Chevallier, L. (2005). «The mass loss of C-rich giants». Astronomy and Astrophysics 429: 235. Bibcode:2005A&A...429..235B. arXiv:astro-ph/0601366. doi:10.1051/0004-6361:20041280. pp. 235-246. 
  40. ↑ «Carina Constellation: Facts, Myth, Star Map, Major Stars, Deep Sky Objects | Constellation Guide». www.constellation-guide.com (en inglés estadounidense). Consultado el 28 de octubre de 2017. 
  41. ↑ Achmad, L. (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. 
  42. ↑ 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. Bibcode:2012ApJ...760...65F. arXiv:1209.6427. doi:10.1088/0004-637X/760/1/65. 
  43. ↑ "Big and Giant Stars"
  44. ↑ http://www.newforestobservatory.com/2012/07/02/the-second-reddest-star-in-the-sky-119-tauri-ce-tauri/
  45. ↑ Van Belle, G. T.; Thompson, R. R.; Creech-Eakman, M. J. (2002). «Angular Size Measurements of Mira Variable Stars at 2.2 Microns. II». The Astronomical Journal 124 (3): 1706. Bibcode:2002AJ....124.1706V. arXiv:astro-ph/0210167. doi:10.1086/342282. 
  46. ↑ «VizieR Detailed Page». Vizier.u-strasbg.fr. Consultado el 14 de octubre de 2012. 
  47. ↑ «VizieR Detailed Page». Vizier.u-strasbg.fr. Consultado el 14 de octubre de 2012. 
  48. ↑ «VizieR Detailed Page». Vizier.u-strasbg.fr. Consultado el 14 de octubre de 2012. 
  49. ↑ Hofmann, K.-H.; Eberhardt, M.; Driebe, T.; Schertl, D.; Scholz, M.; Schoeller, M.; Weigelt, G.; Wittkowski, M. et al. (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. 
  50. ↑ 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. Bibcode:2006ApJ...651.1130G. arXiv:astro-ph/0607158. doi:10.1086/507590. 
  51. ↑ 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. Bibcode:2004A&A...421..703W. arXiv:astro-ph/0404248. doi:10.1051/0004-6361:20035826. 
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