Ова е список на најголемите ѕвезди со познати димензии. Големината е изразена во Сончеви полупречници (прибл. 695.700 км).
Точниот редослед на списокот останува непотполн поради големите недоумици при добивањето на параметрите во пресметките, особено сјајноста и делотворната температура. Многу ѕвездени полупречници можат да се изразат само како просек или во голем вредносен опсег. Вредностите знајачно се разликуваат од еден извор до друг, зависно од брановата должина на набљудување.
Полупречниците на неколку ѕвезди се добиени непосредно по интерферометриски пат. Други се откриени по прикривања (окултации) или од затемнувачки двојки, кои ги испробуваат другите непосредни начини за да ја утврдат вистинската големина. Само неколку корисни суперџиновски ѕвезди подлежат на затскривања од Месечината, какви што се Антарес и Алдебаран. Примери за затемнувачки двојки се Епсилон Кочијаш, VV Кефеј, HR 5171 и црвената џиновска двојка KIC 9246715 во соѕвездието Лебед.[1]
Список
Напомена: Обоените редови се тела наведени за споредба.
↑Hełminiak, K.G.; Ukita, N.; Kambe, E.; Konacki, M. (2015). „Absolute Stellar Parameters of KIC 09246715: A Double-giant Eclipsing System with a Solar-like Oscillator“. The Astrophysical Journal Letters. 813 (2): L25. arXiv:1509.03340. Bibcode:2015ApJ...813L..25H. doi:10.1088/2041-8205/813/2/L25.
↑ 2,02,12,2Arroyo-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.
↑ 4,04,14,24,34,44,54,64,7De 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:1008.1083. Bibcode:2010A&A...523A..18D. doi:10.1051/0004-6361/200913771.
↑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.
↑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.
↑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: L1. arXiv:1309.4086. Bibcode:2014MNRAS.437L...1W. doi:10.1093/mnrasl/slt127.
↑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.
↑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.
↑Wittkowski, M; Abellan, F. J; Arroyo-Torres, B; Chiavassa, A; Guirado, J. C; Marcaide, J. M; Alberdi, A; De Wit, W. J; Hofmann, K.-H; Meilland, A; Millour, F; Mohamed, S; Sanchez-Bermudez, J (28 September 2017). „Multi-epoch VLTI-PIONIER imaging of the supergiant V766 Cen: Image of the close companion in front of the primary“. 1709: arXiv:1709.09430. arXiv:1709.09430. Bibcode:2017arXiv170909430W. Наводот journal бара |journal= (help)
↑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:1308.3580. Bibcode:2013ApJ...774..107K. doi:10.1088/0004-637X/774/2/107.
↑Thompson, R. R.; Creech-Eakman, M. J. (2003). „Interferometric observations of the supergiant S Persei: Evidence for axial symmetry and the warm molecular layer“. American Astronomical Society Meeting 203. 203: 49.07. Bibcode:2003AAS...203.4907T.
↑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:1310.2245. Bibcode:2014MNRAS.437..843G. doi:10.1093/mnras/stt1943.
↑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/0504379. Bibcode:2005A&A...438..273V. doi:10.1051/0004-6361:20042555.
↑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.
↑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. arXiv:1406.5320. Bibcode:2014A&A...568A..85P. doi:10.1051/0004-6361/201423991.
↑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. arXiv:1109.4562. Bibcode:2010ASPC..425..103L.
↑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. arXiv:1406.0001. Bibcode:2014MNRAS.443L..94L. doi:10.1093/mnrasl/slu080.
↑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:1501.01560. Bibcode:2015A&A...575A..50A. doi:10.1051/0004-6361/201425212.
↑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:1405.4032. Bibcode:2014ApJ...785...46B. doi:10.1088/0004-637X/785/1/46.
↑Stickland, D. J. (1985). „IRAS observations of the cool galactic hypergiants“. The Observatory. 105: 229. Bibcode:1985Obs...105..229S.
↑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. Bibcode:2012ApJ...760...65F. doi:10.1088/0004-637X/760/1/65.
↑Wasatonic, Richard P.; Guinan, Edward F.; Durbin, Allyn J. (2015). „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“. Publications of the Astronomical Society of the Pacific. 127 (956): 1010. Bibcode:2015PASP..127.1010W. doi:10.1086/683261.
↑Hawkins, G. W; Skinner, C. J; Meixner, M. M; Jernigan, J. G; Arens, J. F; Keto, E; Graham, J. R (1995). „Discovery of an Extended Nebula around AFGL 2343 (HD 179821) at 10 Microns“. Astrophysical Journal v.452. 452: 314. Bibcode:1995ApJ...452..314H. doi:10.1086/176303.
↑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. arXiv:1304.4800. Bibcode:2013A&A...555A..24O. doi:10.1051/0004-6361/201321063.
↑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.
↑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/0607158. Bibcode:2006ApJ...651.1130G. doi:10.1086/507590.
↑Woodruff, H. C.; Eberhardt, M.; Driebe, T.; Hofmann, K.-H.; и др. (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/0404248. Bibcode:2004A&A...421..703W. doi:10.1051/0004-6361:20035826.
↑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.
↑A. B. Men'shchikov, Y. Balega, T. Blöcker, R. Osterbart, and G.Weigelt (2001). „Structure and physical properties of the rapidly evolving dusty envelope of IRC +10216 reconstructed by detailed two-dimensional radiative transfer modeling“. Astronomy and Astrophysics. arXiv:astro-ph/0206410. Bibcode:2002A&A...392..921M. doi:10.1051/0004-6361:20020954.CS1-одржување: повеќе имиња: список на автори (link)
↑Weigelt, G.; и др. (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/9805022, Bibcode:1998A&A...333L..51W
↑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. стр. 176–191. Bibcode:1995ASPC...83..176L.
↑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.
↑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:1308.1632. Bibcode:2013AJ....146..148M. doi:10.1088/0004-6256/146/6/148.
↑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:1201.0843. Bibcode:2012ApJ...747..108M. doi:10.1088/0004-637X/747/2/108.
↑Chesneau, O.; Kaufer, A.; Stahl, O.; Colvinter, C.; Spang, A.; Dessart, L.; Prinja, R.; Chini, R. (2014). „The variable stellar wind of Rigel probed at high spatial and spectral resolution“. Astronomy & Astrophysics. 566: 18. arXiv:1405.0907. Bibcode:2014A&A...566A.125C. doi:10.1051/0004-6361/201322894. A125.
↑Cruzalebes, 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 (1): 437–450. arXiv:1306.3288. Bibcode:2013MNRAS.434..437C. doi:10.1093/mnras/stt1037.
↑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:1007.3284. Bibcode:2010MNRAS.408..731C. doi:10.1111/j.1365-2966.2010.17167.x.
↑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/0501102, 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.
↑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.
↑Hack, M.; Engin, S.; Yilmaz, N.; Sedmak, G.; Rusconi, L.; Boehm, C. (1992). „Spectroscopic study of the atmospheric eclipsing binary VV Cephei“. Astronomy and Astrophysics Supplement Series (ISSN0365-0138). 95: 589. Bibcode:1992A&AS...95..589H.