Hypergiant - Knowledge (XXG)

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that a small group of hydrogen-rich WNL stars are actually progenitors of blue hypergiants or LBVs. These are the closely related Ofpe (O-type spectra plus H, He, and N emission lines, and other peculiarities) and WN9 (the coolest nitrogen Wolf–Rayet stars) which may be a brief intermediate stage between high mass main-sequence stars and hypergiants or LBVs. Quiescent LBVs have been observed with WNL spectra and apparent Ofpe/WNL stars have changed to show blue hypergiant spectra. High rotation rates cause massive stars to shed their atmospheres quickly and prevent the passage from main sequence to supergiant, so these directly become Wolf–Rayet stars. Wolf Rayet stars, slash stars, cool slash stars (aka WN10/11), Ofpe, Of, and Of stars are not considered hypergiants. Although they are luminous and often have strong emission lines, they have characteristic spectra of their own.

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deeper surface below the outward-moving dense wind. This has been hypothesized to account for the "missing" intermediate-luminosity LBVs and the presence of yellow hypergiants at approximately the same luminosity and cooler temperatures. The yellow hypergiants are actually the LBVs having formed a pseudo-photosphere and so apparently having a lower temperature.

5854: 5880: 5904: 5892: 5134: 618: 479:. Hypergiants are only created in the largest and densest areas of star formation and because of their short lives, only a small number are known despite their extreme luminosity that allows them to be identified even in neighbouring galaxies. The time spent in some phases such as LBVs can be as short as a few thousand years. 440:

temperature. High-mass stars with a high proportion of remaining hydrogen are more stable, while older stars with lower masses and a higher proportion of heavy elements have less stable atmospheres due to increased radiation pressure and decreased gravitational attraction. These are thought to be the hypergiants, near the

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quickly move away from the main sequence and increase somewhat in luminosity to become blue supergiants. They cool and enlarge at approximately constant luminosity to become a red supergiant, then contract and increase in temperature as the outer layers are blown away. They may "bounce" backwards and

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are a class of highly luminous hot stars that display characteristic spectral variation. They often lie in a "quiescent" zone with hotter stars generally being more luminous, but periodically undergo large surface eruptions and move to a narrow zone where stars of all luminosities have approximately

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The yellow hypergiants are thought to be generally post-red supergiant stars that have already lost most of their atmospheres and hydrogen. A few more stable high mass yellow supergiants with approximately the same luminosity are known and thought to be evolving towards the red supergiant phase, but

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as some stars with different classifications. It is not always clear whether the different classifications represent stars with different initial conditions, stars at different stages of an evolutionary track, or is just an artifact of our observations. Astrophysical models explaining the phenomena

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are extremely hot stars that have lost much or all of their outer layers. WNL is a term used for late stage (i.e. cooler) Wolf–Rayet stars with spectra dominated by nitrogen. Although these are generally thought to be the stage reached by hypergiant stars after sufficient mass loss, it is possible

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stars are less luminous than hypergiants of similar temperature, a few fall within the same luminosity range. Ordinary supergiants compared to hypergiants often lack the strong hydrogen emissions whose broadened spectral lines indicate significant mass loss. Evolved lower mass supergiants do not

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Blue hypergiants are found in the same parts of the HR diagram as LBVs but do not necessarily show the LBV variations. Some but not all LBVs show the characteristics of hypergiant spectra at least some of the time, but many authors would exclude all LBVs from the hypergiant class and treat them

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Another theory associated with hypergiant stars is the potential to form a pseudo-photosphere, that is a spherical optically dense surface that is actually formed by the stellar wind rather than being the true surface of the star. Such a pseudo-photosphere would be significantly cooler than the

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of a hypergiant may be nearly strong enough to lift off the photosphere. Above the Eddington limit, the star would generate so much radiation that parts of its outer layers would be thrown off in massive outbursts; this would effectively restrict the star from shining at higher luminosities for

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where hypergiants are found may be newly evolved from the main sequence and still with high mass, or much more evolved post-red supergiant stars that have lost a significant fraction of their initial mass, and these objects cannot be distinguished simply on the basis of their luminosity and

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are simply too luminous to develop a stable extended atmosphere and so they never cool sufficiently to become red supergiants. The most massive stars, especially rapidly rotating stars with enhanced convection and mixing, may skip these steps and move directly to the Wolf–Rayet stage.

361:, indicating an extended stellar atmosphere or a relatively large mass loss rate. The Keenan criterion is the one most commonly used by scientists today; hence it is possible for a supergiant star to have a higher luminosity than a hypergiant of the same spectral class. 3176:

Britavskiy, N. E.; Bonanos, A. Z.; Herrero, A.; Cerviño, M.; García-Álvarez, D.; Boyer, M. L.; Masseron, T.; Mehner, A.; McQuinn, K. B. W. (2019). "Physical parameters of red supergiants in dwarf irregular galaxies in the Local Group".

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Cyril Georgy; Sylvia Ekström; Georges Meynet; Philip Massey; Levesque; Raphael Hirschi; Patrick Eggenberger; André Maeder (2012). "Grids of stellar models with rotation II. WR populations and supernovae/GRB progenitors at Z = 0.014".

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Lagadec, E.; Zijlstra, A. A.; Oudmaijer, R. D.; Verhoelst, T.; Cox, N. L. J.; Szczerba, R.; Mékarnia, D.; Van Winckel, H. (2011). "A double detached shell around a post-red supergiant: IRAS 17163-3907, the Fried Egg nebula".

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Wittkowski, M.; Arroyo-Torres, B.; Marcaide, J. M.; Abellan, F. J.; Chiavassa, A.; Guirado, J. C. (2017). "VLTI/AMBER spectro-interferometry of the late-type supergiants V766 Cen (=HR 5171 A), σ Oph, BM Sco, and HD 206859".

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separately. Blue hypergiants that do not show LBV characteristics may be progenitors of LBVs, or vice versa, or both. Lower mass LBVs may be a transitional stage to or from cool hypergiants or are different type of object.

2124:; Weis, Kerstin; Davidson, Kris; Bomans, D. J.; Burggraf, Birgitta (2014). "Luminous and Variable Stars in M31 and M33. II. Luminous Blue Variables, Candidate LBVs, Fe II Emission Line Stars, and Other Supergiants". 695:. Eta Carinae is extremely massive, possibly as much as 120 to 150 times the mass of the Sun, and is four to five million times as luminous. Possibly a different type of object from the LBVs, or extreme for a LBV. 2180:

Groh, Jose; Meynet, Georges; Ekstrom, Sylvia; Georgy, Cyril (2014). "The evolution of massive stars and their spectra I. A non-rotating 60 Msun star from the zero-age main sequence to the pre-supernova stage".

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Stolovy, S. R.; Cotera, A.; Dong, H.; Morris, M. R.; Wang, Q. D.; Stolovy, S. R.; Lang, C. (2010). "Isolated Wolf-Rayet Stars and O Supergiants in the GalacticCenter Region Identified via Paschen-a Excess".

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these are rare as this is expected to be a rapid transition. Because yellow hypergiants are post-red supergiant stars, there is a fairly hard upper limit to their luminosity at around 500,000–750,000

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in the inner layers, resulting in a density inversion potentially leading to a massive explosion. The theory has, however, not been explored very much, and it is uncertain whether this really can happen.

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are found. Because of their high masses, the lifetime of a hypergiant is very short in astronomical timescales: only a few million years compared to around 10 billion years for stars like the

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Van Genderen, A. M.; Sterken, C. (1999). "Light variations of massive stars (alpha Cygni variables). XVII. The LMC supergiants R 74 (LBV), R 78, HD 34664 = S 22 (B/LBV), R 84 and R 116 (LBV?)".

368:. The use of hydrogen emission lines is not helpful for defining the coolest hypergiants, and these are largely classified by luminosity since mass loss is almost inevitable for the class. 5579: 467:

Almost all hypergiants exhibit variations in luminosity over time due to instabilities within their interiors, but these are small except for two distinct instability regions where

531:. The last time might have been a series of outbursts observed in 1840–1860, reaching mass loss rates much higher than our current understanding of what stellar winds would allow. 2027:

Clark, J. S.; Castro, N.; Garcia, M.; Herrero, A.; Najarro, F.; Negueruela, I.; Ritchie, B. W.; Smith, K. T. (2012). "On the nature of candidate luminous blue variables in M 33".

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Upper portion of H-R Diagram showing the location of the S Doradus instability strip and the location of LBV outbursts. Main sequence is the thin sloping line on the lower left.

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Shenoy, Dinesh; Humphreys, Roberta M.; Jones, Terry J.; Marengo, Massimo; Gehrz, Robert D.; Helton, L. Andrew; Hoffmann, William F.; Skemer, Andrew J.; Hinz, Philip M. (2016).

734:. The Pistol Star is over 25 times more massive than the Sun, and is about 1.7 million times more luminous. Considered a candidate LBV, but variability has not been confirmed. 1541: 2685:

Wolf, B.; Kaufer, A.; Rivinius, T.; Stahl, O.; Szeifert, T.; Tubbesing, S.; Schmid, H. M. (2000). "Spectroscopic Monitoring of Luminous Hot Stars of the Magellanic Clouds".

499:, which is the luminosity at which the radiation pressure expanding the star outward equals the force of the star's gravity collapsing the star inward. This means that the 580:

is the idea of a deeply situated hydrodynamic explosion, blasting off parts of the star's outer layers. The idea is that the star, even at luminosities below the

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are found, with some overlap. It is not clear whether yellow hypergiants ever manage to get past the instability void to become LBVs or explode as a supernova.

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Sterken, C.; de Groot, M.; van Genderen, A. M. (1998). "Cyclicities in the Light Variations of Luminzus Blue Variables II. R40 developing an S Doradus phase".

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show many areas of agreement. Yet there are some distinctions that are not necessarily helpful in establishing relationships between different types of stars.

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Hypergiants are difficult to study due to their rarity. Many hypergiants have highly variable spectra, but they are grouped here into broad spectral classes.

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Nieuwenhuijzen, H; de Jager, C (2000). "Checking the yellow evolutionary void. Three evolutionary critical Hypergiants: HD 33579, HR 8752 & IRC +10420".

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Owocki, S. P.; Gayley, K. G.; Shaviv, N. J. (2004). "A porosity-length formalism for photon-tiring limited mass loss from stars above the Eddington limit".

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Langer, Norbert; Heger, Alexander; García-Segura, Guillermo (1998). "Massive Stars: The Pre-Supernova Evolution of Internal and Circumstellar Structure".

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Hypergiants are expected to have a characteristic broadening and red-shifting of their spectral lines, producing a distinctive spectral shape known as a

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are interested in these stars because they relate to understanding stellar evolution, especially star formation, stability, and their expected demise as

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Clark, J. S.; Najarro, F.; Negueruela, I.; Ritchie, B. W.; Urbaneja, M. A.; Howarth, I. D. (2012). "On the nature of the galactic early-B hypergiants".

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Samus', N. N.; Kazarovets, E. V.; Durlevich, O. V.; Kireeva, N. N.; Pastukhova, E. N. (2017). "General catalogue of variable stars: Version GCVS 5.1".

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Alcolea, J.; Bujarrabal, V.; Planesas, P.; Teyssier, D.; Cernicharo, J.; De Beck, E.; Decin, L.; Dominik, C.; Justtanont, K. (2013-10-09). "HIFISTARS

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Tabernero, H. M.; Dorda, R.; Negueruela, I.; Marfil, E. (February 2021). "The nature of VX Sagitarii: Is it a TŻO, a RSG, or a high-mass AGB star?".

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Zhang, B.; Reid, M. J.; Menten, K. M.; Zheng, X. W. (January 2012). "Distance and Kinematics of the Red Hypergiant VY CMa: VLBA and VLA Astrometry".

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with emission spectra. More commonly, hypergiants are classed as Ia-0 or Ia, but red supergiants are rarely assigned these spectral classifications.

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Clark, J. S.; Negueruela, I.; Crowther, P. A.; Goodwin, S. P. (2005). "On the massive stellar population of the super star cluster Westerlund 1".

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the same temperature, around 8,000 K (13,940 °F; 7,730 °C). This "active" zone is near the hot edge of the unstable "void" where

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K to M type spectra, the largest known stars by radius. Hypergiant luminosity classes are rarely applied to red supergiants, although the term

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Smith, N.; Owocki, S. P. (2006). "On the role of continuum driven eruptions in the evolution of very massive stars and population III stars".

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Clark, J. S.; Negueruela, I.; Gonzalez-Fernandez, C. (2013). "IRAS 18357-0604 - an analogue of the galactic yellow hypergiant IRC +10420?".

5171: 263:. However, this is rarely seen in literature or in published spectral classifications, except for specific well-defined groups such as the 5789: 4981: 4300: 2602:

Kathryn F. Neugent; Philip Massey; Brian Skiff; Georges Meynet (April 2012). "Yellow and Red Supergiants in the Magellanic Clouds".

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Groh, J. H.; Meynet, G.; Ekström, S. (2013). "Massive star evolution: Luminous blue variables as unexpected supernova progenitors".

561:. This is important, since most massive stars also are very metal-poor, which means that the effect must work independently of the 5574: 4693: 602: 436: 36: 5610: 1181:

Plus at least two probable cool hypergiants in the recently discovered Scutum Red Supergiant Clusters: F15 and possibly F13 in

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Yellow hypergiants typically have late A to early K spectra. However, A-type hypergiants can also be called white hypergiants.

5551: 4607: 5819: 5234: 4986: 4623: 3642: 376: 5033: 4900: 2658:

Van Genderen, A. M.; Jones, A.; Sterken, C. (2006). "Light variations of alpha Cygni variables in the Magellanic Clouds".

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Brott, I.; Evans, C. J.; Hunter, I.; De Koter, A.; Langer, N.; Dufton, P. L.; Cantiello, M.; Trundle, C.; Lennon, D. J.;

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is sometimes applied to the most extended and unstable red supergiants, with radii on the order of 1,000 to 2,000

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superimposed on an outline of the Solar System. The blue half-ring centered near the left edge represents the orbit of

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Skiff, B. A. (2014). "VizieR Online Data Catalog: Catalogue of Stellar Spectral Classifications (Skiff, 2009-2016)".

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As the luminosity of stars increases greatly with mass, the luminosity of hypergiants often lies very close to the

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Owocki, S. P.; Van Marle, Allard Jan (2007). "Luminous Blue Variables & Mass Loss near the Eddington Limit".

5804: 5799: 5164: 4171: 4045: 3680: 565:. In the same line of reasoning, the continuum driving may also contribute to an upper mass limit even for the 5244: 4698: 4367: 2506:

Maíz Apellániz, J.; Negueruela, I. (30 July 2024). "Barbá 2: A new supergiant-rich Galactic stellar cluster".

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Some luminous blue variables are classified as hypergiants, during at least part of their cycle of variation:

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Hypergiants are evolved, high luminosity, high-mass stars that occur in the same or similar regions of the

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forwards executing one or more "blue loops", still at a fairly steady luminosity, until they explode as a

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will be larger for very cool and very hot stars, for example at least −9.7 for a B0 hypergiant). In 1971,

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Mauron, N.; Josselin, E. (2011). "The mass-loss rates of red supergiants and the de Jager prescription".

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return from the red supergiant phase, either exploding as supernovae or leaving behind a white dwarf.

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Jura, M.; Velusamy, T.; Werner, M. W. (2001). "What Next for the Likely Presupernova HD 179821?".

1347: 5908: 5600: 5509: 5485: 5377: 5337: 5199: 5098: 5059: 5011: 4996: 4910: 4850: 4773: 4683: 4653: 4643: 4587: 4509: 4200: 3836: 3635: 3589: 3562: 3536: 3469: 3438: 3412: 3383: 3357: 3251: 3212: 3186: 3158: 3132: 3105: 3079: 3048: 3022: 2955: 2929: 2902: 2876: 2848: 2822: 2792: 2766: 2637: 2611: 2577: 2551: 2507: 2322: 2296: 2269: 2243: 2216: 2190: 2159: 2133: 2082:"Warm Dust around Blue Hypergiants: Mid-Infrared Imaging of the Luminous Blue Variable HD 168625" 2062: 2036: 1928: 1882: 1859: 1748: 1712: 1686: 1660: 1631: 1605: 1576: 1550: 1521: 1495: 1464: 1438: 1410: 938: 933: 332: 324: 206: 3232:"SEARCHING FOR COOL DUST IN THE MID-TO-FAR INFRARED: THE MASS-LOSS HISTORIES OF THE HYPERGIANTS 916: 894: 1046: 900: 888: 882: 876: 5636: 5480: 5410: 5347: 5259: 5209: 5194: 5049: 4534: 4474: 4447: 4427: 4227: 4011: 3999: 3826: 3806: 3760: 3742: 3710: 3342: 3318: 3070:; Marengo, M. (2006). "The Circumstellar Environments of NML Cygni and the Cool Hypergiants". 1918: 1738: 1152: 1068: 1012: 864: 630: 472: 264: 2481:

VizieR On-line Data Catalog: B/Mk. Originally Published in: Lowell Observatory (October 2014)

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because of its extreme luminosity, although it has not shown the characteristic variability.

1262: 1208: 1083: 953: 813: 808: 803: 660: 449: 393: 304: 798: 5427: 5332: 5064: 4867: 4736: 4580: 4551: 4492: 4487: 4362: 4090: 4055: 3989: 3935: 3930: 3875: 3685: 1199: 1073: 1057: 1052: 763: 585: 581: 528: 496: 385: 296: 288: 185: 3513: 3426: 3306: 3290: 3265: 3146: 3093: 2990: 2780: 2698: 2671: 2625: 2492: 2366: 2310: 2147: 2097: 1963: 1896: 1810: 1779: 1726: 1674: 1619: 1564: 5459: 5415: 5389: 5126: 4892: 4731: 4558: 4529: 4504: 4437: 4126: 3994: 3880: 3782: 3672: 3662: 1344: 1273: 1193: 566: 539: 500: 268: 192: 2788: 2633: 5918: 5663: 5078: 4872: 4835: 4803: 4678: 4387: 4210: 4181: 4159: 3777: 3750: 3727: 3628: 3566: 3442: 3434: 3274: 3231: 3216: 2852: 2641: 2326: 2287:

Bianchi, Luciana; Bohlin, Ralph; Massey, Philip (2004). "The Ofpe/WN9 Stars in M33".

2273: 2220: 2163: 2155: 1863: 1483: 1468: 1414: 1100: 1094: 1088: 948: 927: 839: 684: 141: 3387: 3343:"The distance and size of the red hypergiant NML Cygni from VLBA and VLA astrometry" 3162: 3109: 3052: 2959: 2906: 2796: 2581: 2066: 1932: 1752: 1690: 1580: 1525: 515:, one of the most massive stars ever observed. With an estimated mass of around 130 5896: 5641: 5541: 5514: 5492: 5138: 4813: 4763: 4758: 4658: 4541: 4524: 4482: 4442: 4377: 4260: 4205: 4186: 4166: 4144: 4136: 3979: 3972: 3811: 3732: 3715: 1635: 1288: 1228: 1186: 1125: 1105: 1078: 978: 784: 535: 516: 401: 248: 178: 106: 99: 92: 85: 78: 71: 64: 57: 50: 3611: 3558: 3483: 3379: 3208: 3044: 2951: 2898: 2573: 2265: 2212: 2058: 1517: 1460: 2844: 1914: 1734: 538:(that is, ones driven by absorbing light from the star in huge numbers of narrow 27:

Rare star with tremendous luminosity and high rates of mass loss by stellar winds

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Stickland, D. J. (1985). "IRAS observations of the cool galactic hypergiants".

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Zhang, B.; Reid, M. J.; Menten, K. M.; Zheng, X. W.; Brunthaler, A. (2012).

1982: 1311: 1278: 1252: 1246: 1241: 1216: 1118: 943: 829: 753: 742: 737: 712: 457:, but blue hypergiants can be much more luminous, sometimes several million 417: 300: 280: 164: 127: 1881:. Astrophysics and Space Science Library. Vol. 384. pp. 221–247. 1711:. Astrophysics and Space Science Library. Vol. 384. pp. 221–247. 1486:; Yoon, S. -C.; Anders, P. (2011). "Rotating massive main-sequence stars". 17: 2741: 1855: 1406: 723:. Prototype variable, LBVs are still sometimes called S Doradus variables. 5723: 5688: 5683: 5678: 5502: 5342: 4818: 4519: 4193: 3952: 3925: 3137: 3084: 2827: 2301: 1665: 1610: 1283: 1268: 1257: 1110: 1040: 858: 852: 688: 570: 550: 299:, a yellow hypergiant that is one of the brightest to the naked eye; and 150: 134: 5698: 5668: 5646: 5093: 4568: 4330: 4097: 4050: 4033: 4028: 3947: 1877:

Vink, Jorick S. (2012). "Eta Carinae and the Luminous Blue Variables".

1173: 1166: 1023: 780: 730:(V4647 Sgr), near the center of the Milky Way, in the constellation of 698: 397: 365: 358: 272: 1948:"Yellow Hypergiants as Dynamically Unstable Post–Red Supergiant Stars" 5693: 5497: 5083: 5071: 4290: 4176: 2512: 833: 554: 3474: 5891: 5133: 3594: 3314: 3256: 3191: 3154: 3101: 3027: 2998: 2974: 2318: 2106: 2081: 1972: 1947: 1819: 1794: 1707:

Vink, J. S. (2012). "Eta Carinae and the Luminous Blue Variables".

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Miroshnichenko, A. S.; Chentsov, E. L.; Klochkova, V. G. (2000).

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Another theory to explain the massive outbursts of, for example,

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Relationships with Ofpe, WNL, LBV, and other supergiant stars

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A good candidate for hosting a continuum-driven wind is

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Timeline of white dwarfs, neutron stars, and supernovae

930:(= MWC 314), LBV candidate with a supergiant companion. 2687:

Thermal and Ionization Aspects of Flows from Hot Stars

542:), continuum driving does not require the presence of 5868: 3291:"Luminosities of the M-Type Variables of Small Range" 1834:

De Jager, Cornelis (1998). "The yellow hypergiants".

897:(R81 in LMC), LBV candidate, eclipsing binary system. 5767: 5629: 5588: 5562: 5473: 5398: 5310: 5252: 5187: 5042: 4891: 4789: 4717: 4616: 4473: 4348: 4226: 4135: 3862: 3741: 3671: 1542:

Proceedings of the International Astronomical Union

420:or completely shed their outer layers to become a 331:(later changed into hypergiant) for stars with an 247:, mass, size and mass loss because of its extreme 2975:"Revised MK spectral types for G, K, and M stars" 790:Usually B-class, occasionally late O or early A: 783:proto-planetary disk compared to the size of the 424:. Stars with an initial mass above about 40 357:showing at least one broad emission component in 2537: 2535: 2533: 2531: 2529: 2527: 2525: 2523: 519:and a luminosity four million times that of the 1383:de Jager, C. (1998). "The Yellow Hypergiants". 1265:- potentially the largest star in the Milky Way 705:. Prototype for the general characteristics of 491:Great nebula in Carina, surrounding Eta Carinae 408:Stars with an initial mass above about 25 353:suggested that the term would be used only for 283:. Notable examples of hypergiants include the 5165: 3636: 2808: 2806: 2653: 2651: 1022:Field surrounding the yellow hypergiant star 8: 5795:Monte Agliale Supernovae and Asteroid Survey 3495: 3493: 3336: 3334: 3332: 2721:Astronomy and Astrophysics Supplement Series 1203:Size comparison between the diameter of the 2979:The Astrophysical Journal Supplement Series 2175: 2173: 573:, which did not contain any metals at all. 5172: 5158: 5150: 3868: 3643: 3629: 3621: 557:, which have few such lines — in the 3593: 3540: 3473: 3460:/HIFI observations of VY Canis Majoris". 3416: 3361: 3273: 3255: 3190: 3136: 3083: 3026: 2933: 2880: 2826: 2770: 2740: 2615: 2555: 2511: 2474: 2472: 2470: 2468: 2466: 2464: 2462: 2460: 2458: 2300: 2247: 2194: 2137: 2105: 2040: 1981: 1971: 1904: 1886: 1818: 1716: 1664: 1609: 1554: 1499: 1442: 287:, a blue hypergiant located close to the 2456: 2454: 2452: 2450: 2448: 2446: 2444: 2442: 2440: 2438: 435:This means that stars at the top of the 5875: 2597: 2595: 2593: 2591: 2348: 2346: 2344: 2342: 2340: 2338: 2336: 1995: 1993: 1879:Eta Carinae and the Supernova Impostors 1709:Eta Carinae and the Supernova Impostors 1375: 1330:Some authors consider Cygnus OB2-12 an 1323: 380:Comparison of (from left to right) the 832:(Wray 977 or GX 301-2), binary with a 5210:Type II (IIP, IIL, IIn, and IIb) 1946:Stothers, R. B.; Chin, C. W. (2001). 1702: 1700: 1386:The Astronomy and Astrophysics Review 7: 5853: 2973:Keenan, P. C.; Pitts, R. E. (1980). 2080:Robberto, M.; Herbst, T. M. (1998). 5790:Katzman Automatic Imaging Telescope 1363:May just be a closer post-AGB star. 1091:(HR 5171A, possible red supergiant) 766:on the other side of the Milky Way. 719:, in the southern constellation of 701:, in the northern constellation of 691:) in the southern constellation of 2714:"AS314: A dusty A-type hypergiant" 1793:Stothers, N.; Chin, C.-W. (1996). 25: 1836:Astronomy and Astrophysics Review 523:, astrophysicists speculate that 5902: 5890: 5878: 5852: 5843: 5842: 5575:History of supernova observation 5243: 5132: 5122: 5121: 3289:Keenan, Philip C. (1942-05-01). 2660:The Journal of Astronomical Data 30: 5820:SuperNova Early Warning System 5235:Common envelope jets supernova 400:, the outermost planet of the 307:'s "Garnet Star"), one of the 1: 5034:Timeline of stellar astronomy 1307:Lists of astronomical objects 1215:(possibly the largest in the 1213:among the largest known stars 659:image of the surroundings of 5810:Supernova/Acceleration Probe 5785:High-Z Supernova Search Team 5383:pulsational pair-instability 3582:Astronomy & Astrophysics 3462:Astronomy & Astrophysics 3350:Astronomy & Astrophysics 3236:Cep, VY CMa, IRC+10420, AND 3179:Astronomy & Astrophysics 3015:Astronomy & Astrophysics 2922:Astronomy & Astrophysics 2869:Astronomy & Astrophysics 2544:Astronomy & Astrophysics 2236:Astronomy & Astrophysics 2183:Astronomy & Astrophysics 2029:Astronomy & Astrophysics 1915:10.1007/978-1-4614-2275-4_10 1735:10.1007/978-1-4614-2275-4_10 1488:Astronomy & Astrophysics 1431:Astronomy & Astrophysics 527:may occasionally exceed the 5815:Supernova Cosmology Project 5323:Fast blue optical transient 4694:Hertzsprung–Russell diagram 3612:10.1051/0004-6361/202039236 3559:10.1051/0004-6361/201013993 3484:10.1051/0004-6361/201321683 3380:10.1051/0004-6361/201219587 3209:10.1051/0004-6361/201935212 3045:10.1051/0004-6361/201629349 2952:10.1051/0004-6361/201322772 2899:10.1051/0004-6361/201117521 2789:10.1088/0004-637X/725/1/188 2634:10.1088/0004-637X/749/2/177 2574:10.1051/0004-6361/201117472 2266:10.1051/0004-6361/201220741 2213:10.1051/0004-6361/201322573 2059:10.1051/0004-6361/201118440 1768:Reviews in Modern Astronomy 1518:10.1051/0004-6361/201016114 1461:10.1051/0004-6361/201118340 960:In Galactic Center Region: 603:Hertzsprung–Russell diagram 437:Hertzsprung–Russell diagram 311:and brightest stars known. 243:that has an extremely high 38:Hertzsprung–Russell diagram 5951: 4608:Kelvin–Helmholtz mechanism 3529:Astronomy and Astrophysics 3435:10.1088/0004-637X/744/1/23 3275:10.3847/0004-6256/151/3/51 2845:10.1051/0004-6361:20042413 2815:Astronomy and Astrophysics 2417:Astronomy and Astrophysics 2390:Astronomy and Astrophysics 2156:10.1088/0004-637X/790/1/48 2002:Astronomy and Astrophysics 1302:List of most massive stars 779:A hypergiant star and its 584:, would have insufficient 534:As opposed to line-driven 5838: 5241: 5117: 3871: 3658: 3404:The Astrophysical Journal 3295:The Astrophysical Journal 3125:The Astrophysical Journal 2759:The Astrophysical Journal 2375:10.1134/S1063772917010085 2289:The Astrophysical Journal 2126:The Astrophysical Journal 2086:The Astrophysical Journal 1952:The Astrophysical Journal 1799:The Astrophysical Journal 1652:The Astrophysical Journal 1597:The Astrophysical Journal 1573:10.1017/S1743921308020358 567:first generation of stars 549: — atoms other than 444:and rapidly losing mass. 319:In 1956, the astronomers 293:most luminous stars known 239:) is a very rare type of 29: 5800:Nearby Supernova Factory 4987:With multiple exoplanets 3244:The Astronomical Journal 3072:The Astronomical Journal 1211:, a hypergiant which is 1160:LGGS J013250.70+304510.6 985:W5 (possible Wolf–Rayet) 5825:Supernova Legacy Survey 3773:Asymptotic giant branch 3604:2021A&A...646A..98T 3551:2011A&A...526A.156M 3372:2012A&A...544A..42Z 3201:2019A&A...631A..95B 3037:2017A&A...597A...9W 2944:2014A&A...561A..15C 2891:2011A&A...534L..10L 2837:2005A&A...434..949C 2733:2000A&AS..144..379M 2566:2012A&A...541A.145C 2429:1999A&A...349..537V 2402:1998A&A...333..565S 2258:2013A&A...550L...7G 2205:2014A&A...564A..30G 2051:2012A&A...541A.146C 2014:2000A&A...353..163N 1848:1998A&ARv...8..145D 1510:2011A&A...530A.116B 1453:2012A&A...542A..29G 1399:1998A&ARv...8..145D 973:, type O, LBV candidate 967:, type O, LBV candidate 671:Luminous blue variables 626:Luminous blue variables 469:luminous blue variables 5830:Texas Supernova Search 5805:Sloan Supernova Survey 5423:Luminous blue variable 5109:Tidal disruption event 4598:Circumstellar envelope 3832:Luminous blue variable 1343:Brightest star of the 1220: 1026: 787: 717:Large Magellanic Cloud 663: 622: 492: 405: 5275:Phillips relationship 4634:Effective temperature 2604:Astrophysical Journal 2122:Humphreys, Roberta M. 1856:10.1007/s001590050009 1407:10.1007/s001590050009 1202: 1021: 778: 655: 620: 490: 379: 315:Origin and definition 5104:Planet-hosting stars 4982:With resolved images 4953:Historical brightest 4883:Photometric-standard 4809:Solar radio emission 4603:Eddington luminosity 4383:Triple-alpha process 4321:Thorne–Żytkow object 3696:Young stellar object 657:Very Large Telescope 503:passing through the 5848:Category:Supernovae 5780:Calán/Tololo Survey 5465:Population III star 5373:Soft gamma repeater 5205:Type Ib and Ic 4928:Highest temperature 4699:Color–color diagram 4564:Protoplanetary disk 4368:Proton–proton chain 4046:Chemically peculiar 3514:1985Obs...105..229S 3427:2012ApJ...744...23Z 3307:1942ApJ....95..461K 3266:2016AJ....151...51S 3147:2001ApJ...556..408J 3094:2006AJ....131..603S 2991:1980ApJS...42..541K 2781:2010ApJ...725..188M 2742:10.1051/aas:2000216 2699:2000ASPC..204...43W 2672:2006JAD....12....4V 2626:2012ApJ...749..177N 2493:2014yCat....1.2023S 2367:2017ARep...61...80S 2311:2004ApJ...601..228B 2148:2014ApJ...790...48H 2098:1998ApJ...498..400R 1964:2001ApJ...560..934S 1897:2012ASSL..384..221V 1811:1996ApJ...468..842S 1780:1998RvMA...11...57L 1727:2012ASSL..384..221V 1675:2006ApJ...645L..45S 1620:2004ApJ...616..525O 1565:2008IAUS..250...71O 1115:Variable A (in M33) 756:, (R116 in the LMC) 5858:Commons:Supernovae 5510:Stellar black hole 5486:Pulsar wind nebula 5338:Gravitational wave 4933:Lowest temperature 4684:Photometric system 4654:Absolute magnitude 4588:Circumstellar dust 4201:Stellar black hole 3837:Stellar population 3723:Herbig–Haro object 1221: 1027: 1013:Yellow hypergiants 788: 664: 631:yellow hypergiants 623: 493: 473:yellow hypergiants 406: 333:absolute magnitude 265:yellow hypergiants 5935:Stellar phenomena 5866: 5865: 5481:Supernova remnant 5348:Luminous red nova 5260:Carbon detonation 5147: 5146: 5050:Substellar object 5029:Planetary nebulae 4448:Luminous red nova 4358:Deuterium burning 4344: 4343: 3827:Instability strip 3807:Wolf-Rayet nebula 3761:Horizontal branch 3706:Pre-main-sequence 3066:Schuster, M. T.; 2355:Astronomy Reports 1924:978-1-4614-2274-7 1744:978-1-4614-2274-7 1153:Triangulum Galaxy 1069:Omicron1 Centauri 648:Known hypergiants 16:(Redirected from 5942: 5907: 5906: 5905: 5895: 5894: 5883: 5882: 5881: 5874: 5856: 5855: 5846: 5845: 5709:Remnant G1.9+0.3 5328:Fast radio burst 5247: 5225:Pair-instability 5174: 5167: 5160: 5151: 5139:Stars portal 5137: 5136: 5125: 5124: 4781:Planetary system 4704:Strömgren sphere 4576:Asteroseismology 4297:Black hole star 3869: 3795:Planetary nebula 3756:Red-giant branch 3645: 3638: 3631: 3622: 3616: 3615: 3597: 3577: 3571: 3570: 3544: 3524: 3518: 3517: 3497: 3488: 3487: 3477: 3453: 3447: 3446: 3420: 3398: 3392: 3391: 3365: 3347: 3338: 3327: 3326: 3286: 3280: 3279: 3277: 3259: 3227: 3221: 3220: 3194: 3173: 3167: 3166: 3140: 3138:astro-ph/0103282 3120: 3114: 3113: 3087: 3085:astro-ph/0510010 3068:Humphreys, R. M. 3063: 3057: 3056: 3030: 3009: 3003: 3002: 2970: 2964: 2963: 2937: 2917: 2911: 2910: 2884: 2863: 2857: 2856: 2830: 2828:astro-ph/0504342 2810: 2801: 2800: 2774: 2753: 2747: 2746: 2744: 2718: 2709: 2703: 2702: 2682: 2676: 2675: 2655: 2646: 2645: 2619: 2599: 2586: 2585: 2559: 2539: 2518: 2517: 2515: 2503: 2497: 2496: 2476: 2433: 2432: 2412: 2406: 2405: 2385: 2379: 2378: 2350: 2331: 2330: 2304: 2302:astro-ph/0310187 2284: 2278: 2277: 2251: 2231: 2225: 2224: 2198: 2177: 2168: 2167: 2141: 2118: 2112: 2111: 2109: 2077: 2071: 2070: 2044: 2024: 2018: 2017: 1997: 1988: 1987: 1985: 1983:2060/20010083764 1975: 1943: 1937: 1936: 1908: 1890: 1874: 1868: 1867: 1831: 1825: 1824: 1822: 1790: 1784: 1783: 1763: 1757: 1756: 1720: 1704: 1695: 1694: 1668: 1666:astro-ph/0606174 1646: 1640: 1639: 1613: 1611:astro-ph/0409573 1591: 1585: 1584: 1558: 1536: 1530: 1529: 1503: 1479: 1473: 1472: 1446: 1425: 1419: 1418: 1380: 1364: 1361: 1355: 1341: 1335: 1328: 1263:VY Canis Majoris 1209:VY Canis Majoris 1084:V509 Cassiopeiae 944:V4030 Sagittarii 867:, LBV candidate` 771:Blue hypergiants 738:V4029 Sagittarii 661:VY Canis Majoris 641:Wolf–Rayet stars 569:right after the 508:longer periods. 394:VY Canis Majoris 329:super-supergiant 273:B(e) supergiants 259:0 (zero) in the 257:luminosity class 230:luminosity class 219: 202: 195: 188: 181: 174: 167: 160: 153: 146: 137: 130: 123: 116: 109: 102: 95: 88: 81: 74: 67: 60: 53: 46: 39: 34: 21: 5950: 5949: 5945: 5944: 5943: 5941: 5940: 5939: 5915: 5914: 5913: 5903: 5901: 5889: 5879: 5877: 5869: 5867: 5862: 5834: 5763: 5749:SN 2016aps 5729:SN Refsdal 5625: 5584: 5558: 5469: 5455:Wolf–Rayet star 5394: 5333:Gamma-ray burst 5306: 5280:Nucleosynthesis 5248: 5239: 5183: 5178: 5148: 5143: 5131: 5113: 5038: 5007:Milky Way novae 4943:Smallest volume 4887: 4868:Radial velocity 4791: 4785: 4737:Common envelope 4713: 4612: 4581:Helioseismology 4552:Bipolar outflow 4493:Microturbulence 4488:Convection zone 4469: 4363:Lithium burning 4350:Nucleosynthesis 4340: 4222: 4131: 3858: 3737: 3686:Molecular cloud 3667: 3654: 3649: 3619: 3579: 3578: 3574: 3526: 3525: 3521: 3502:The Observatory 3499: 3498: 3491: 3455: 3454: 3450: 3400: 3399: 3395: 3345: 3340: 3339: 3330: 3288: 3287: 3283: 3229: 3228: 3224: 3175: 3174: 3170: 3122: 3121: 3117: 3065: 3064: 3060: 3011: 3010: 3006: 2972: 2971: 2967: 2919: 2918: 2914: 2865: 2864: 2860: 2812: 2811: 2804: 2755: 2754: 2750: 2716: 2711: 2710: 2706: 2684: 2683: 2679: 2657: 2656: 2649: 2601: 2600: 2589: 2541: 2540: 2521: 2505: 2504: 2500: 2478: 2477: 2436: 2414: 2413: 2409: 2387: 2386: 2382: 2352: 2351: 2334: 2286: 2285: 2281: 2233: 2232: 2228: 2179: 2178: 2171: 2120: 2119: 2115: 2079: 2078: 2074: 2026: 2025: 2021: 1999: 1998: 1991: 1945: 1944: 1940: 1925: 1906:10.1.1.250.4184 1876: 1875: 1871: 1833: 1832: 1828: 1792: 1791: 1787: 1765: 1764: 1760: 1745: 1706: 1705: 1698: 1648: 1647: 1643: 1593: 1592: 1588: 1538: 1537: 1533: 1481: 1480: 1476: 1427: 1426: 1422: 1382: 1381: 1377: 1373: 1368: 1367: 1362: 1358: 1342: 1338: 1329: 1325: 1320: 1298: 1293: 1234: 1231: 1197: 1194:Red hypergiants 1185:and Star 49 in 1179: 1074:Rho Cassiopeiae 1058:IRAS 18357-0604 1053:IRAS 17163-3907 1016: 1009: 959: 924:, LBV candidate 773: 764:1806-20 cluster 709:spectral lines. 674: 650: 599: 586:heat convection 582:Eddington limit 529:Eddington limit 497:Eddington limit 485: 463: 460: 455: 452: 442:Eddington limit 430: 427: 422:Wolf–Rayet star 414: 411: 386:Rho Cassiopeiae 374: 366:P Cygni profile 348: 341: 317: 297:Rho Cassiopeiae 291:and one of the 289:Galactic Center 269:red supergiants 222: 221: 217: 213: 211: 209: 207: 204: 200: 197: 193: 190: 186: 183: 179: 176: 172: 169: 165: 162: 158: 155: 151: 148: 144: 142: 139: 135: 132: 128: 125: 121: 118: 114: 111: 107: 104: 100: 97: 93: 90: 86: 83: 79: 76: 72: 69: 65: 62: 58: 55: 51: 48: 44: 41: 37: 28: 23: 22: 15: 12: 11: 5: 5948: 5946: 5938: 5937: 5932: 5927: 5917: 5916: 5912: 5911: 5899: 5887: 5864: 5863: 5861: 5860: 5850: 5839: 5836: 5835: 5833: 5832: 5827: 5822: 5817: 5812: 5807: 5802: 5797: 5792: 5787: 5782: 5777: 5771: 5769: 5765: 5764: 5762: 5761: 5756: 5751: 5746: 5741: 5739:SN 2006gy 5736: 5731: 5726: 5721: 5719:SN 2011fe 5716: 5714:SN 2007bi 5711: 5706: 5704:SN 2003fg 5701: 5696: 5691: 5686: 5681: 5676: 5671: 5666: 5661: 5656: 5655: 5654: 5644: 5639: 5637:Barnard's Loop 5633: 5631: 5627: 5626: 5624: 5623: 5618: 5613: 5608: 5603: 5598: 5592: 5590: 5586: 5585: 5583: 5582: 5577: 5572: 5566: 5564: 5560: 5559: 5557: 5556: 5555: 5554: 5552:Orion–Eridanus 5544: 5539: 5534: 5533: 5532: 5527: 5522: 5512: 5507: 5506: 5505: 5500: 5490: 5489: 5488: 5477: 5475: 5471: 5470: 5468: 5467: 5462: 5460:Super-AGB star 5457: 5452: 5447: 5446: 5445: 5440: 5435: 5425: 5420: 5419: 5418: 5413: 5402: 5400: 5396: 5395: 5393: 5392: 5390:Symbiotic nova 5387: 5386: 5385: 5375: 5370: 5365: 5360: 5355: 5350: 5345: 5340: 5335: 5330: 5325: 5320: 5314: 5312: 5308: 5307: 5305: 5304: 5299: 5298: 5297: 5292: 5287: 5277: 5272: 5267: 5262: 5256: 5254: 5250: 5249: 5242: 5240: 5238: 5237: 5232: 5227: 5222: 5217: 5212: 5207: 5202: 5197: 5191: 5189: 5185: 5184: 5179: 5177: 5176: 5169: 5162: 5154: 5145: 5144: 5142: 5141: 5129: 5118: 5115: 5114: 5112: 5111: 5106: 5101: 5096: 5091: 5086: 5081: 5076: 5075: 5074: 5069: 5068: 5067: 5062: 5046: 5044: 5040: 5039: 5037: 5036: 5031: 5026: 5025: 5024: 5019: 5009: 5004: 4999: 4994: 4989: 4984: 4979: 4978: 4977: 4972: 4971: 4970: 4960: 4955: 4950: 4945: 4940: 4938:Largest volume 4935: 4930: 4925: 4915: 4914: 4913: 4908: 4897: 4895: 4889: 4888: 4886: 4885: 4880: 4875: 4870: 4865: 4864: 4863: 4858: 4853: 4843: 4838: 4833: 4828: 4823: 4822: 4821: 4816: 4811: 4806: 4795: 4793: 4787: 4786: 4784: 4783: 4778: 4777: 4776: 4771: 4766: 4756: 4751: 4750: 4749: 4744: 4739: 4734: 4723: 4721: 4715: 4714: 4712: 4711: 4706: 4701: 4696: 4691: 4686: 4681: 4676: 4671: 4666: 4661: 4656: 4651: 4649:Magnetic field 4646: 4641: 4636: 4631: 4626: 4620: 4618: 4614: 4613: 4611: 4610: 4605: 4600: 4595: 4590: 4585: 4584: 4583: 4573: 4572: 4571: 4566: 4559:Accretion disk 4556: 4555: 4554: 4549: 4539: 4538: 4537: 4535:Alfvén surface 4532: 4530:Stellar corona 4527: 4522: 4517: 4507: 4505:Radiation zone 4502: 4501: 4500: 4495: 4485: 4479: 4477: 4471: 4470: 4468: 4467: 4462: 4461: 4460: 4455: 4450: 4445: 4440: 4430: 4425: 4420: 4415: 4410: 4405: 4400: 4395: 4390: 4385: 4380: 4375: 4370: 4365: 4360: 4354: 4352: 4346: 4345: 4342: 4341: 4339: 4338: 4333: 4328: 4323: 4318: 4313: 4312: 4311: 4306: 4303: 4295: 4294: 4293: 4288: 4283: 4278: 4273: 4268: 4263: 4258: 4253: 4243: 4238: 4232: 4230: 4224: 4223: 4221: 4220: 4215: 4214: 4213: 4203: 4198: 4197: 4196: 4191: 4190: 4189: 4184: 4174: 4164: 4163: 4162: 4152: 4147: 4141: 4139: 4133: 4132: 4130: 4129: 4127:Blue straggler 4124: 4123: 4122: 4112: 4107: 4106: 4105: 4095: 4094: 4093: 4088: 4083: 4078: 4073: 4068: 4063: 4058: 4053: 4043: 4038: 4037: 4036: 4031: 4026: 4016: 4015: 4014: 4004: 4003: 4002: 3997: 3992: 3982: 3977: 3976: 3975: 3970: 3965: 3955: 3950: 3945: 3940: 3939: 3938: 3933: 3923: 3922: 3921: 3916: 3911: 3906: 3901: 3896: 3891: 3885:Main sequence 3883: 3878: 3872: 3866: 3864:Classification 3860: 3859: 3857: 3856: 3855: 3854: 3849: 3839: 3834: 3829: 3824: 3819: 3814: 3809: 3804: 3803: 3802: 3800:Protoplanetary 3792: 3787: 3786: 3785: 3780: 3770: 3769: 3768: 3758: 3753: 3747: 3745: 3739: 3738: 3736: 3735: 3730: 3725: 3720: 3719: 3718: 3713: 3708: 3703: 3693: 3688: 3683: 3677: 3675: 3669: 3668: 3666: 3665: 3659: 3656: 3655: 3650: 3648: 3647: 3640: 3633: 3625: 3618: 3617: 3572: 3519: 3489: 3448: 3393: 3328: 3315:10.1086/144418 3281: 3222: 3168: 3155:10.1086/321553 3115: 3102:10.1086/498395 3078:(1): 603–611. 3058: 3004: 2999:10.1086/190662 2965: 2912: 2858: 2802: 2765:(1): 188–199. 2748: 2704: 2677: 2647: 2587: 2519: 2498: 2434: 2407: 2380: 2332: 2319:10.1086/380485 2295:(1): 228–241. 2279: 2226: 2169: 2113: 2107:10.1086/305519 2092:(1): 400–412. 2072: 2019: 1989: 1973:10.1086/322438 1938: 1923: 1869: 1842:(3): 145–180. 1826: 1820:10.1086/177740 1785: 1758: 1743: 1696: 1683:10.1086/506523 1659:(1): L45–L48. 1641: 1628:10.1086/424910 1604:(1): 525–541. 1586: 1531: 1484:De Mink, S. E. 1474: 1420: 1393:(3): 145–180. 1374: 1372: 1369: 1366: 1365: 1356: 1345:OB association 1336: 1322: 1321: 1319: 1316: 1315: 1314: 1309: 1304: 1297: 1294: 1292: 1291: 1286: 1281: 1276: 1274:PZ Cassiopeiae 1271: 1266: 1260: 1255: 1250: 1244: 1238: 1232: 1229: 1225:red hypergiant 1196: 1191: 1178: 1177: 1163: 1162: 1149: 1148: 1145: 1142: 1139: 1136: 1133: 1122: 1121: 1116: 1113: 1108: 1103: 1098: 1092: 1086: 1081: 1076: 1071: 1066: 1060: 1055: 1050: 1044: 1038: 1031: 1015: 1010: 1008: 1007: 1004: 1001: 998: 995: 992: 989: 986: 975: 974: 968: 957: 956: 951: 946: 941: 936: 931: 925: 919: 914: 911: 908: 903: 898: 892: 886: 880: 874: 868: 862: 856: 850: 842: 837: 827: 821: 816: 811: 806: 801: 796: 792: 772: 769: 768: 767: 757: 751: 750:, (R40 in SMC) 745: 740: 735: 724: 710: 696: 673: 668: 649: 646: 609:Although most 598: 595: 540:spectral lines 501:radiative flux 484: 481: 461: 458: 453: 450: 428: 425: 412: 409: 373: 370: 346: 339: 335:brighter than 327:used the term 316: 313: 255:is defined as 215: 205: 198: 194:Red supergiant 191: 184: 177: 170: 163: 156: 149: 140: 133: 126: 119: 112: 105: 98: 91: 84: 77: 70: 63: 56: 49: 42: 35: 26: 24: 14: 13: 10: 9: 6: 4: 3: 2: 5947: 5936: 5933: 5931: 5928: 5926: 5923: 5922: 5920: 5910: 5900: 5898: 5893: 5888: 5886: 5876: 5872: 5859: 5851: 5849: 5841: 5840: 5837: 5831: 5828: 5826: 5823: 5821: 5818: 5816: 5813: 5811: 5808: 5806: 5803: 5801: 5798: 5796: 5793: 5791: 5788: 5786: 5783: 5781: 5778: 5776: 5773: 5772: 5770: 5766: 5760: 5757: 5755: 5752: 5750: 5747: 5745: 5742: 5740: 5737: 5735: 5732: 5730: 5727: 5725: 5724:SN 2014J 5722: 5720: 5717: 5715: 5712: 5710: 5707: 5705: 5702: 5700: 5697: 5695: 5692: 5690: 5689:SN 1994D 5687: 5685: 5684:SN 1987A 5682: 5680: 5679:SN 1885A 5677: 5675: 5672: 5670: 5667: 5665: 5662: 5660: 5657: 5653: 5650: 5649: 5648: 5645: 5643: 5640: 5638: 5635: 5634: 5632: 5628: 5622: 5619: 5617: 5614: 5612: 5609: 5607: 5606:Massive stars 5604: 5602: 5599: 5597: 5594: 5593: 5591: 5587: 5581: 5578: 5576: 5573: 5571: 5568: 5567: 5565: 5561: 5553: 5550: 5549: 5548: 5545: 5543: 5540: 5538: 5535: 5531: 5528: 5526: 5523: 5521: 5518: 5517: 5516: 5513: 5511: 5508: 5504: 5501: 5499: 5496: 5495: 5494: 5491: 5487: 5484: 5483: 5482: 5479: 5478: 5476: 5472: 5466: 5463: 5461: 5458: 5456: 5453: 5451: 5448: 5444: 5441: 5439: 5436: 5434: 5431: 5430: 5429: 5426: 5424: 5421: 5417: 5414: 5412: 5409: 5408: 5407: 5404: 5403: 5401: 5397: 5391: 5388: 5384: 5381: 5380: 5379: 5376: 5374: 5371: 5369: 5366: 5364: 5361: 5359: 5356: 5354: 5351: 5349: 5346: 5344: 5341: 5339: 5336: 5334: 5331: 5329: 5326: 5324: 5321: 5319: 5316: 5315: 5313: 5309: 5303: 5300: 5296: 5293: 5291: 5288: 5286: 5283: 5282: 5281: 5278: 5276: 5273: 5271: 5268: 5266: 5263: 5261: 5258: 5257: 5255: 5251: 5246: 5236: 5233: 5231: 5228: 5226: 5223: 5221: 5220:Superluminous 5218: 5216: 5213: 5211: 5208: 5206: 5203: 5201: 5200:Type Iax 5198: 5196: 5193: 5192: 5190: 5186: 5182: 5175: 5170: 5168: 5163: 5161: 5156: 5155: 5152: 5140: 5135: 5130: 5128: 5120: 5119: 5116: 5110: 5107: 5105: 5102: 5100: 5099:Intergalactic 5097: 5095: 5092: 5090: 5087: 5085: 5082: 5080: 5079:Galactic year 5077: 5073: 5070: 5066: 5063: 5061: 5058: 5057: 5056: 5053: 5052: 5051: 5048: 5047: 5045: 5041: 5035: 5032: 5030: 5027: 5023: 5020: 5018: 5015: 5014: 5013: 5010: 5008: 5005: 5003: 5000: 4998: 4995: 4993: 4990: 4988: 4985: 4983: 4980: 4976: 4973: 4969: 4966: 4965: 4964: 4961: 4959: 4958:Most luminous 4956: 4954: 4951: 4949: 4946: 4944: 4941: 4939: 4936: 4934: 4931: 4929: 4926: 4924: 4921: 4920: 4919: 4916: 4912: 4909: 4907: 4904: 4903: 4902: 4899: 4898: 4896: 4894: 4890: 4884: 4881: 4879: 4876: 4874: 4873:Proper motion 4871: 4869: 4866: 4862: 4859: 4857: 4854: 4852: 4849: 4848: 4847: 4844: 4842: 4839: 4837: 4836:Constellation 4834: 4832: 4829: 4827: 4824: 4820: 4817: 4815: 4812: 4810: 4807: 4805: 4804:Solar eclipse 4802: 4801: 4800: 4797: 4796: 4794: 4790:Earth-centric 4788: 4782: 4779: 4775: 4772: 4770: 4767: 4765: 4762: 4761: 4760: 4757: 4755: 4752: 4748: 4745: 4743: 4740: 4738: 4735: 4733: 4730: 4729: 4728: 4725: 4724: 4722: 4720: 4716: 4710: 4707: 4705: 4702: 4700: 4697: 4695: 4692: 4690: 4687: 4685: 4682: 4680: 4677: 4675: 4672: 4670: 4667: 4665: 4662: 4660: 4657: 4655: 4652: 4650: 4647: 4645: 4642: 4640: 4637: 4635: 4632: 4630: 4627: 4625: 4622: 4621: 4619: 4615: 4609: 4606: 4604: 4601: 4599: 4596: 4594: 4591: 4589: 4586: 4582: 4579: 4578: 4577: 4574: 4570: 4567: 4565: 4562: 4561: 4560: 4557: 4553: 4550: 4548: 4545: 4544: 4543: 4540: 4536: 4533: 4531: 4528: 4526: 4523: 4521: 4518: 4516: 4513: 4512: 4511: 4508: 4506: 4503: 4499: 4496: 4494: 4491: 4490: 4489: 4486: 4484: 4481: 4480: 4478: 4476: 4472: 4466: 4463: 4459: 4456: 4454: 4451: 4449: 4446: 4444: 4441: 4439: 4436: 4435: 4434: 4431: 4429: 4426: 4424: 4421: 4419: 4416: 4414: 4411: 4409: 4406: 4404: 4401: 4399: 4396: 4394: 4391: 4389: 4388:Alpha process 4386: 4384: 4381: 4379: 4376: 4374: 4371: 4369: 4366: 4364: 4361: 4359: 4356: 4355: 4353: 4351: 4347: 4337: 4334: 4332: 4329: 4327: 4324: 4322: 4319: 4317: 4314: 4310: 4307: 4304: 4302: 4299: 4298: 4296: 4292: 4289: 4287: 4284: 4282: 4279: 4277: 4274: 4272: 4269: 4267: 4264: 4262: 4259: 4257: 4254: 4252: 4249: 4248: 4247: 4244: 4242: 4239: 4237: 4234: 4233: 4231: 4229: 4225: 4219: 4216: 4212: 4209: 4208: 4207: 4204: 4202: 4199: 4195: 4192: 4188: 4185: 4183: 4180: 4179: 4178: 4175: 4173: 4170: 4169: 4168: 4165: 4161: 4160:Helium planet 4158: 4157: 4156: 4153: 4151: 4150:Parker's star 4148: 4146: 4143: 4142: 4140: 4138: 4134: 4128: 4125: 4121: 4118: 4117: 4116: 4113: 4111: 4108: 4104: 4101: 4100: 4099: 4096: 4092: 4089: 4087: 4084: 4082: 4081:Lambda Boötis 4079: 4077: 4074: 4072: 4069: 4067: 4064: 4062: 4059: 4057: 4054: 4052: 4049: 4048: 4047: 4044: 4042: 4039: 4035: 4032: 4030: 4027: 4025: 4022: 4021: 4020: 4017: 4013: 4010: 4009: 4008: 4005: 4001: 3998: 3996: 3993: 3991: 3988: 3987: 3986: 3983: 3981: 3978: 3974: 3971: 3969: 3966: 3964: 3961: 3960: 3959: 3956: 3954: 3951: 3949: 3946: 3944: 3941: 3937: 3934: 3932: 3929: 3928: 3927: 3924: 3920: 3917: 3915: 3912: 3910: 3907: 3905: 3902: 3900: 3897: 3895: 3892: 3890: 3887: 3886: 3884: 3882: 3879: 3877: 3874: 3873: 3870: 3867: 3865: 3861: 3853: 3850: 3848: 3847:Superluminous 3845: 3844: 3843: 3840: 3838: 3835: 3833: 3830: 3828: 3825: 3823: 3820: 3818: 3815: 3813: 3810: 3808: 3805: 3801: 3798: 3797: 3796: 3793: 3791: 3788: 3784: 3781: 3779: 3776: 3775: 3774: 3771: 3767: 3764: 3763: 3762: 3759: 3757: 3754: 3752: 3751:Main sequence 3749: 3748: 3746: 3744: 3740: 3734: 3731: 3729: 3728:Hayashi track 3726: 3724: 3721: 3717: 3714: 3712: 3709: 3707: 3704: 3702: 3699: 3698: 3697: 3694: 3692: 3689: 3687: 3684: 3682: 3679: 3678: 3676: 3674: 3670: 3664: 3661: 3660: 3657: 3653: 3646: 3641: 3639: 3634: 3632: 3627: 3626: 3623: 3613: 3609: 3605: 3601: 3596: 3591: 3587: 3583: 3576: 3573: 3568: 3564: 3560: 3556: 3552: 3548: 3543: 3538: 3534: 3530: 3523: 3520: 3515: 3511: 3507: 3503: 3496: 3494: 3490: 3485: 3481: 3476: 3471: 3467: 3463: 3459: 3452: 3449: 3444: 3440: 3436: 3432: 3428: 3424: 3419: 3414: 3410: 3406: 3405: 3397: 3394: 3389: 3385: 3381: 3377: 3373: 3369: 3364: 3359: 3355: 3351: 3344: 3337: 3335: 3333: 3329: 3324: 3320: 3316: 3312: 3308: 3304: 3300: 3296: 3292: 3285: 3282: 3276: 3271: 3267: 3263: 3258: 3253: 3249: 3245: 3241: 3239: 3235: 3226: 3223: 3218: 3214: 3210: 3206: 3202: 3198: 3193: 3188: 3184: 3180: 3172: 3169: 3164: 3160: 3156: 3152: 3148: 3144: 3139: 3134: 3130: 3126: 3119: 3116: 3111: 3107: 3103: 3099: 3095: 3091: 3086: 3081: 3077: 3073: 3069: 3062: 3059: 3054: 3050: 3046: 3042: 3038: 3034: 3029: 3024: 3020: 3016: 3008: 3005: 3000: 2996: 2992: 2988: 2984: 2980: 2976: 2969: 2966: 2961: 2957: 2953: 2949: 2945: 2941: 2936: 2931: 2927: 2923: 2916: 2913: 2908: 2904: 2900: 2896: 2892: 2888: 2883: 2878: 2874: 2870: 2862: 2859: 2854: 2850: 2846: 2842: 2838: 2834: 2829: 2824: 2820: 2816: 2809: 2807: 2803: 2798: 2794: 2790: 2786: 2782: 2778: 2773: 2768: 2764: 2760: 2752: 2749: 2743: 2738: 2734: 2730: 2726: 2722: 2715: 2708: 2705: 2700: 2696: 2692: 2688: 2681: 2678: 2673: 2669: 2665: 2661: 2654: 2652: 2648: 2643: 2639: 2635: 2631: 2627: 2623: 2618: 2613: 2609: 2605: 2598: 2596: 2594: 2592: 2588: 2583: 2579: 2575: 2571: 2567: 2563: 2558: 2553: 2549: 2545: 2538: 2536: 2534: 2532: 2530: 2528: 2526: 2524: 2520: 2514: 2509: 2502: 2499: 2494: 2490: 2486: 2482: 2475: 2473: 2471: 2469: 2467: 2465: 2463: 2461: 2459: 2457: 2455: 2453: 2451: 2449: 2447: 2445: 2443: 2441: 2439: 2435: 2430: 2426: 2422: 2418: 2411: 2408: 2403: 2399: 2395: 2391: 2384: 2381: 2376: 2372: 2368: 2364: 2360: 2356: 2349: 2347: 2345: 2343: 2341: 2339: 2337: 2333: 2328: 2324: 2320: 2316: 2312: 2308: 2303: 2298: 2294: 2290: 2283: 2280: 2275: 2271: 2267: 2263: 2259: 2255: 2250: 2245: 2241: 2237: 2230: 2227: 2222: 2218: 2214: 2210: 2206: 2202: 2197: 2192: 2188: 2184: 2176: 2174: 2170: 2165: 2161: 2157: 2153: 2149: 2145: 2140: 2135: 2131: 2127: 2123: 2117: 2114: 2108: 2103: 2099: 2095: 2091: 2087: 2083: 2076: 2073: 2068: 2064: 2060: 2056: 2052: 2048: 2043: 2038: 2034: 2030: 2023: 2020: 2015: 2011: 2007: 2003: 1996: 1994: 1990: 1984: 1979: 1974: 1969: 1965: 1961: 1957: 1953: 1949: 1942: 1939: 1934: 1930: 1926: 1920: 1916: 1912: 1907: 1902: 1898: 1894: 1889: 1884: 1880: 1873: 1870: 1865: 1861: 1857: 1853: 1849: 1845: 1841: 1837: 1830: 1827: 1821: 1816: 1812: 1808: 1804: 1800: 1796: 1789: 1786: 1781: 1777: 1773: 1769: 1762: 1759: 1754: 1750: 1746: 1740: 1736: 1732: 1728: 1724: 1719: 1714: 1710: 1703: 1701: 1697: 1692: 1688: 1684: 1680: 1676: 1672: 1667: 1662: 1658: 1654: 1653: 1645: 1642: 1637: 1633: 1629: 1625: 1621: 1617: 1612: 1607: 1603: 1599: 1598: 1590: 1587: 1582: 1578: 1574: 1570: 1566: 1562: 1557: 1552: 1548: 1544: 1543: 1535: 1532: 1527: 1523: 1519: 1515: 1511: 1507: 1502: 1497: 1493: 1489: 1485: 1478: 1475: 1470: 1466: 1462: 1458: 1454: 1450: 1445: 1440: 1436: 1432: 1424: 1421: 1416: 1412: 1408: 1404: 1400: 1396: 1392: 1388: 1387: 1379: 1376: 1370: 1360: 1357: 1353: 1349: 1346: 1340: 1337: 1333: 1327: 1324: 1317: 1313: 1310: 1308: 1305: 1303: 1300: 1299: 1295: 1290: 1287: 1285: 1282: 1280: 1277: 1275: 1272: 1270: 1267: 1264: 1261: 1259: 1256: 1254: 1251: 1248: 1245: 1243: 1240: 1239: 1237: 1235: 1226: 1218: 1214: 1210: 1206: 1201: 1195: 1192: 1190: 1188: 1184: 1175: 1172: 1171: 1170: 1168: 1161: 1158: 1157: 1156: 1154: 1146: 1143: 1140: 1137: 1134: 1131: 1130: 1129: 1127: 1120: 1117: 1114: 1112: 1109: 1107: 1104: 1102: 1101:V1427 Aquilae 1099: 1096: 1095:V810 Centauri 1093: 1090: 1089:V766 Centauri 1087: 1085: 1082: 1080: 1077: 1075: 1072: 1070: 1067: 1064: 1061: 1059: 1056: 1054: 1051: 1048: 1045: 1042: 1039: 1036: 1033: 1032: 1030: 1025: 1020: 1014: 1011: 1005: 1002: 999: 996: 993: 991:W13 (binary?) 990: 987: 984: 983: 982: 980: 972: 969: 966: 963: 962: 961: 955: 954:Zeta¹ Scorpii 952: 950: 949:6 Cassiopeiae 947: 945: 942: 940: 937: 935: 932: 929: 928:V1429 Aquilae 926: 923: 920: 918: 915: 912: 909: 907: 904: 902: 899: 896: 893: 890: 887: 885:(R111 in LMC) 884: 881: 878: 875: 872: 869: 866: 863: 861:(R126 in LMC) 860: 857: 854: 851: 849: 846: 843: 841: 840:Cygnus OB2-12 838: 835: 831: 828: 825: 822: 820: 817: 815: 812: 810: 807: 805: 802: 800: 797: 794: 793: 791: 786: 782: 777: 770: 765: 761: 758: 755: 752: 749: 746: 744: 741: 739: 736: 733: 729: 725: 722: 718: 714: 711: 708: 704: 700: 697: 694: 690: 686: 685:Carina Nebula 683:, inside the 682: 679: 678: 677: 672: 669: 667: 662: 658: 654: 647: 645: 642: 638: 634: 632: 627: 619: 615: 612: 607: 604: 596: 594: 590: 587: 583: 579: 574: 572: 568: 564: 560: 556: 552: 548: 545: 541: 537: 536:stellar winds 532: 530: 526: 522: 518: 514: 509: 506: 502: 498: 489: 482: 480: 478: 474: 470: 465: 456: 445: 443: 438: 433: 423: 419: 403: 399: 395: 391: 387: 383: 378: 371: 369: 367: 362: 360: 356: 352: 345: 338: 334: 330: 326: 322: 314: 312: 310: 306: 302: 298: 294: 290: 286: 282: 278: 274: 270: 266: 262: 258: 254: 250: 249:stellar winds 246: 242: 238: 234: 231: 227: 220: 203: 196: 189: 182: 180:Bright giants 175: 168: 161: 154: 147: 143:Main sequence 138: 131: 124: 117: 110: 103: 96: 89: 82: 75: 68: 61: 54: 47: 45:Spectral type 40: 33: 19: 5734:Vela Remnant 5699:SN 1006 5664:SN 1000+0216 5642:Cassiopeia A 5611:Most distant 5542:Local Bubble 5515:Compact star 5493:Neutron star 5405: 5230:Calcium-rich 5195:Type Ia 5002:White dwarfs 4992:Brown dwarfs 4975:Most distant 4923:Most massive 4901:Proper names 4861:Photographic 4814:Solar System 4792:observations 4719:Star systems 4542:Stellar wind 4525:Chromosphere 4498:Oscillations 4378:Helium flash 4228:Hypothetical 4206:X-ray binary 4145:Compact star 4006: 3980:Bright giant 3733:Henyey track 3711:Herbig Ae/Be 3585: 3581: 3575: 3532: 3528: 3522: 3505: 3501: 3465: 3461: 3457: 3451: 3408: 3402: 3396: 3353: 3349: 3298: 3294: 3284: 3247: 3243: 3237: 3233: 3225: 3182: 3178: 3171: 3128: 3124: 3118: 3075: 3071: 3061: 3018: 3014: 3007: 2982: 2978: 2968: 2925: 2921: 2915: 2872: 2868: 2861: 2818: 2814: 2762: 2758: 2751: 2724: 2720: 2707: 2690: 2686: 2680: 2663: 2659: 2607: 2603: 2547: 2543: 2513:2407.20812v2 2501: 2484: 2480: 2420: 2416: 2410: 2393: 2389: 2383: 2358: 2354: 2292: 2288: 2282: 2239: 2235: 2229: 2186: 2182: 2129: 2125: 2116: 2089: 2085: 2075: 2032: 2028: 2022: 2005: 2001: 1955: 1951: 1941: 1878: 1872: 1839: 1835: 1829: 1802: 1798: 1788: 1771: 1767: 1761: 1708: 1656: 1650: 1644: 1601: 1595: 1589: 1546: 1540: 1534: 1491: 1487: 1477: 1434: 1430: 1423: 1390: 1384: 1378: 1359: 1348:Scorpius OB1 1339: 1326: 1289:V602 Carinae 1224: 1222: 1180: 1164: 1150: 1126:Westerlund 1 1123: 1106:V915 Scorpii 1079:V382 Carinae 1049:(R59 in LMC) 1037:(R45 in SMC) 1028: 979:Westerlund 1 976: 958: 910:M33 OB21 108 873:(R66 in LMC) 855:(R62 in LMC) 847: 789: 785:Solar System 743:V905 Scorpii 675: 665: 639: 635: 624: 608: 600: 591: 575: 533: 517:solar masses 510: 494: 466: 446: 434: 407: 402:Solar System 363: 343: 336: 328: 318: 252: 236: 232: 225: 223: 199: 122:White dwarfs 115:Brown dwarfs 5925:Hypergiants 5909:Outer space 5744:ASASSN-15lh 5694:SN 185 5652:Crab Nebula 5547:Superbubble 5537:Zombie star 5520:electroweak 5450:White dwarf 5399:Progenitors 5363:Pulsar kick 5055:Brown dwarf 4831:Circumpolar 4709:Kraft break 4689:Color index 4664:Metallicity 4624:Designation 4593:Cosmic dust 4515:Photosphere 4281:Dark-energy 4256:Electroweak 4241:Black dwarf 4172:Radio-quiet 4155:White dwarf 4041:White dwarf 3691:Bok globule 3475:1310.2400v1 2008:: 163–176. 1805:: 842–850. 1065:(V1302 Aql) 939:V2140 Cygni 934:V1768 Cygni 906:HT Sagittae 760:LBV 1806-20 732:Sagittarius 728:Pistol Star 681:Eta Carinae 578:Eta Carinae 563:metallicity 559:photosphere 525:Eta Carinae 513:Eta Carinae 505:photosphere 471:(LBVs) and 382:Pistol Star 355:supergiants 285:Pistol Star 277:Astronomers 271:), or blue 251:. The term 201:Hypergiants 187:Supergiants 173:Blue giants 18:Hypergiants 5930:Star types 5919:Categories 5759:SN 2022jli 5754:SN 2018cow 5621:In fiction 5596:Candidates 5570:Guest star 5428:Supergiant 5406:Hypergiant 5368:Quark-nova 5270:Near-Earth 5253:Physics of 5181:Supernovae 5017:Candidates 5012:Supernovae 4997:Red dwarfs 4856:Extinction 4644:Kinematics 4639:Luminosity 4617:Properties 4510:Atmosphere 4408:Si burning 4398:Ne burning 4336:White hole 4309:Quasi-star 4236:Blue dwarf 4091:Technetium 4007:Hypergiant 3985:Supergiant 3595:2011.09184 3257:1512.01529 3192:1909.13378 3131:(1): 408. 3028:1610.01927 2821:(3): 949. 2727:(3): 379. 2610:(2): 177. 1958:(2): 934. 1371:References 1354:candidate. 922:V452 Scuti 917:V430 Scuti 895:HDE 269128 836:companion. 611:supergiant 544:"metallic" 390:Betelgeuse 281:supernovae 261:MKK system 253:hypergiant 245:luminosity 226:hypergiant 166:Red giants 145:("dwarfs") 129:Red dwarfs 5885:Astronomy 5659:iPTF14hls 5563:Discovery 5353:Micronova 5302:Neutrinos 5295:γ-process 5290:r-process 5285:p-process 5265:Foe/Bethe 5215:Hypernova 4948:Brightest 4846:Magnitude 4826:Pole star 4747:Symbiotic 4742:Eclipsing 4674:Starlight 4475:Structure 4465:Supernova 4458:Micronova 4453:Recurrent 4438:Symbiotic 4423:p-process 4418:r-process 4413:s-process 4403:O burning 4393:C burning 4373:CNO cycle 4316:Gravastar 3852:Hypernova 3842:Supernova 3817:Dredge-up 3790:Blue loop 3783:super-AGB 3766:Red clump 3743:Evolution 3701:Protostar 3681:Accretion 3673:Formation 3567:119276502 3542:1010.5369 3443:121202336 3418:1109.3036 3411:(1): 23. 3363:1207.1850 3323:0004-637X 3250:(3): 51. 3217:203593402 2935:1311.3956 2882:1109.5947 2853:119042919 2772:1009.2769 2642:119180846 2617:1202.4225 2557:1202.3991 2361:(1): 80. 2327:119371998 2274:119227339 2249:1301.1519 2221:118870118 2196:1401.7322 2164:119177378 2139:1407.2259 2132:(1): 48. 2042:1202.4409 1901:CiteSeerX 1888:0905.3338 1864:189936279 1718:0905.3338 1556:0801.2519 1549:: 71–83. 1501:1102.0766 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