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List of largest stars

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

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

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

Caveats

UY Scuti as seen in visible light.

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

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

Extragalactic large stars

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

List

List of the largest stars
Star name Solar radii
(Sun = 1)
Method[a] Notes
Orbit of Saturn 1,940–2,169 Reported for reference
UY Scuti 1,708 ± 192[3] AD The quoted size was based on an angular diameter and distance of 2.9 kpc. Gaia Data Release 2 suggests a much closer distance and consequently smaller radius.
WOH G64 1,540[4]–1,730[5] L/Teff This would be the largest star in the LMC, but is unusual in position and motion and might still be a foreground halo giant.
RW Cephei 1,535[6][7] L/Teff RW Cep is variable both in brightness (by at least a factor of 3) and spectral type (observed from G8 to M), thus probably also in diameter. Because the spectral type and temperature at maximum luminosity are not known, the quoted size is just an estimate.
Westerlund 1-26 1,530–1,580[8] (–2,550) [9] L/Teff Very uncertain parameters for an unusual star with strong radio emission. The spectrum is variable but apparently the luminosity is not.
HD 143183 1,480[10]–1,830[11] L/Teff
VY Canis Majoris 1,420 ± 120[12] AD The size of VY CMa was revised in 2012 through newly improved measurements[13] which result this value being the highest among well-characterized stars.[14] Other stars could be larger but they could have less accurate radius estimates.
KY Cygni 1,420–2,850 [1] L/Teff 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.
AH Scorpii 1,411 ± 124[3] AD 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.
RSGC1-F02 1,398[15] L/Teff
IRAS 04509-6922 1,360[16] L/Teff
RSGC1-F01 1,335[15] L/Teff
HR 5171 A 1,315 ± 260,[17] 1,575 ± 400[18] AD HR 5171 A is a highly distorted star in a close binary system, losing mass to the secondary, and is also variable in temperature, thus probably also in diameter. Traditionally, it is considered as the largest known yellow hypergiant, although the latest research suggests it is a red supergiant with a radius of 1,490 ± 540 R.[19]
SMC 18136 1,310[2] Largest star in the Small Magellanic Cloud
IRAS 05280-6910 1,260[16] - 1,738[20] L/Teff
Mu Cephei (Herschel's "Garnet Star") 1,260[21] Prototype of the obsolete class of the Mu Cephei variables and also the reddest star in the night sky in terms of the B-V color index.[22] Other recent estimates range from 650 R[23] to 1,420 R[1]
LMC 136042 1,240[2]
BI Cygni 1,240[1] L/Teff
Westerlund 1-237 1,233[9] L/Teff
SMC 5092 1,220[2]
S Persei 1,212 ± 124[24] AD & L/Teff A red hypergiant localed in the Perseus Double Cluster. A large radius of 1,230 R is due to an unusual K-band measurement and thought to be an artifact of a reddening correction error. A small radius of 780 R is consistent with other stars in the same survey and with theoretical models.[1]
LMC 175464 1,200[2]
LMC 135720 1,200[2]
IRC-10414 1,200[25] IRC -10414 is a rare red supergiant companion to WR 114 that has a bow shock.
PZ Cassiopeiae 1,190–1,940[1] L/Teff The upper estimate is due to an unusual K-band measurement and thought to be an artefact of a reddening correction error. The lower estimate is consistent with other stars in the same survey and with theoretical models, and the intermediate ones have been obtained refining the distance to this star, and thus its parameters.[26]
SMC 69886 1,190[2]
NML Cygni 1,183[27] L/Teff
RSGC1-F05 1,177[15] L/Teff
EV Carinae 1,168[28]-2,880[29] L/Teff
RSGC1-F03 1,168[15] L/Teff
LMC 119219 1,150[2]
RSGC1-F08 1,146[15] L/Teff
BC Cygni 1,140[1]-1,230[21] L/Teff BC Cyg is calculated to vary in size from 856 R to 1,553 R.[30]
MY Cephei 1,134[31] L/Teff One of the coolest known red supergiants.
SMC 10889 1,130[2]
VX Sagittarii 1,120 - 1,550[32] L/Teff VX Sgr is a pulsating variable calculated to vary in size from 1,350 R to 1,940 R.[33]
LMC 141430 1,110[2]
IRAS 04516-6902 1,100[16] L/Teff
LMC 175746 1,100[2]
RSGC1-F13 1,098[15] L/Teff
RT Carinae 1,090[1] L/Teff
RSGC1-F04 1,082[15] L/Teff
LMC 174714 1,080[2]
LMC 68125 1,080[2]
SMC 49478 1,080[2]
SMC 20133 1,080[2]
V396 Centauri 1,070[1] L/Teff
SMC 8930 1,070[2]
Orbit of Jupiter 1,064–1,173 Reported for reference
HV 11423 1,060–1,220[34] L/Teff 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[1] L/Teff
SMC 25879 1,060[2]
VV Cephei A 1,050[35] - 1,900[1] VV Cep A is a highly distorted star in a close binary system, losing mass to the secondary for at least part of its orbit. Data from the most recent eclipse has cast additional doubt on the accepted model of the system. It is among the largest stars visible to the naked eye.
LMC 142202 1,050[2]
LMC 146126 1,050[2]
LMC 67982 1,040[2]
U Lacertae 1,022[36][37] L/Teff
RSGC1-F11 1,015[15] L/Teff
W Persei 1,011[9] L/Teff
LMC 143877 1,010[2]
KW Sagittarii 1,009[3]-1,460[1] AD & L/Teff Margin of possible error: ±142 R.[3]
RSGC1-F12 1,005[9] L/Teff
Progenitor of SN 2017eaw 1,000–2,000[38] Localed in NGC 6946
SMC 46497 990[2]
LMC 140296 990[2]
RSGC1-F09 986[15] L/Teff
NR Vulpeculae 980[1] L/Teff
SMC 12322 980[2]
LMC 177997 980[2]
SMC 59803 970[2]
Westerlund 1-20 965[9] L/Teff
GCIRS 7 960[39]–1,000[40] AD At the galactic center. Margin of possible error: ±92 R[39] or ±150 R.[40]
Betelgeuse (Alpha Orionis) 955±217[41] AD Star with the third largest apparent size after R Doradus and the Sun. Other estimates range from 887 ± 203 R[42] to 1,180 R[43]
SMC 50840 950[2]
J004424.94+412322.3 945–1,300[44] L/Teff Located in the Andromeda Galaxy.
RSGC1-F10 931[15] L/Teff
S Cassiopeiae 930[45][46]
IX Carinae 920[1] L/Teff
HV 2112 916[47] L/Teff Most likely candidate for a Thorne-Zytkow Object.
RSGC1-F07 910[15] L/Teff
LMC 54365 900[2]
IRAS 04498-6842 900[48]–1,660[16] L/Teff
NSV 25875 891[27] L/Teff
LMC 109106 890[2]
RSGC1-F06 885[15] L/Teff
LMC 116895 880[2]
SMC 30616 880[2]
LMC 64048 880[2]
IRAS 05558-7000 880[16] L/Teff
V437 Scuti 874[27] L/Teff
IRAS 04407-7000 870[16] L/Teff
IRAS 05329-6708 870[16] L/Teff
V602 Carinae 860[1]–1,050[49] L/Teff & AD Margin of possible error: ±165 R.[49]
J004047.82+410936.4 860[44] L/Teff Localed in the Andromeda Galaxy
J004428.71+420601.6 860[44] L/Teff Localed in the Andromeda Galaxy
V669 Cassiopeiae 859[27] L/Teff
SMC 55681 850[2]
SMC 15510 850[2]
LMC 61753 830[2]
LMC 62090 830[2]
SMC 11709 830[2]
V1185 Scorpii 830[27] L/Teff
LMC 142199 810[2]
IRAS 05294-7104 810[16] L/Teff
IRAS 05402-6956 800[16] L/Teff
LMC 134383 800[2]
Eta Carinae A (Tseen She) 800[50] Previously thought to be the most massive single star, but in 2005 it was realized to be a binary system. During the Great Eruption, the size was as large as 1,400 R.[51]
V441 Persei 799[9] L/Teff
BU Persei 795[9] L/Teff
IRAS 05298-6957 790[16] L/Teff
BO Carinae 790[1] L/Teff
LMC 142907 790[2]
J004359.94+411330.9 785[44] L/Teff Localed in the Andromeda Galaxy
SU Persei 780[1] L/Teff In the Perseus Double Cluster
RS Persei 770[52]–1,000[1] AD & L/Teff In the Perseus Double Cluster. Margin of possible error: ±30 R.[52]
AV Persei 770[1] L/Teff In the Perseus Double Cluster
V355 Cephei 770[1] L/Teff Mauron et al. 2011 derive 37,000 L, which implies a size around 300 R.[36]
J004124.80+411634.7 760[44] L/Teff Localed in the Andromeda Galaxy
V915 Scorpii 760[53][54] L/Teff
S Cephei 760[55] AD
YZ Persei 758[9] L/Teff
J004447.08+412801.7 755[44] L/Teff Localed in the Andromeda Galaxy
GP Cassiopeiae 751[9] L/Teff
Outer limits of the asteroid belt 750–900 Reported for reference
SMC 11939 750[2]
HD 303250 750[1] L/Teff
V382 Carinae 747[56] The brightest yellow hypergiant in the night sky, one of the rarest types of star. Other estimate ranges of 600 R to 1,100 R.[57]
RU Virginis 740[58] L/Teff
LMC 137818 740[2]
SMC 48122 740[2]
IRAS 04545-7000 730[16] L/Teff
IRAS 05003-6712 730[16] L/Teff
SMC 56732 730[2]
KK Persei 724[9] L/Teff
V648 Cassiopeiae 710[1] L/Teff
XX Persei 710[9] L/Teff Located in the Perseus Double Cluster and near the border with Andromeda.
TV Geminorum 620–710[59] (–770)[1] L/Teff
HD 179821 704[60] A yellow hypergiant, although most authors consider it as a supergiant, a protoplanetary nebula or a post-AGB star with a luminosity of only 16,000 L.
J004255.95+404857.5 700[44] L/Teff Localed in the Andromeda Galaxy
J003950.98+405422.5 700[61] L/Teff Localed in the Andromeda Galaxy
LMC 169754 700[2]
LMC 65558 700[2]
V528 Carinae 700[1] L/Teff
RSGC1-F14 700[15] L/Teff
The following well-known stars are listed for the purpose of comparison.
V354 Cephei 690[36]-1,520[1] L/Teff
Antares A (Alpha Scorpii A) 680[62] AD This star appears to vary its size by 165 R. Older estimates have given radii over 800 R,[63][64] but some are likely to have been affected by asymmetry of the atmosphere and the narrow range of infrared wavelengths observed.[62]
HR 5171 Ab 650±150[18] AD Companion of HR 5171 A.
CE Tauri 587–593[65] (–608[66]) AD Second reddest star in the night sky.[22] Can be occulted by the Moon, allowing accurate determination of its apparent diameter.
CW Leonis 500[67]–700[68] L/Teff CW Leonis is one of the mistaken identities as the claimed planet "Nibiru" or "Planet X", due to its brightness as it approaches 1st magnitude. Other estimates range from 390 R[67] to 826 R.[27]
Rho Cassiopeiae 400–500[69] Yellow hypergiant, one of the rarest types of a star.
R Leporis (Hind's "Crimson Star") 400[70]–535[71] Margin of possible error: ±90 R.[70]
V509 Cassiopeiae 400–900[72] Yellow hypergiant, one of the rarest types of a star.
Inner limits of the asteroid belt 380 Reported for reference
V838 Monocerotis 380 (in 2009)[73] A short time after the outburst V838 Mon was measured at 1,570 ± 400 R.[74] However the distance to this "L-type supergiant", and hence its size, have since been reduced and it proved to be a transient object that shrunk about four-fold over a few years. Like CW Leo, it has been erroneously portrayed as "Nibiru" or "Planet X" (see above).
R Doradus 370±50[75] Star with the second largest apparent size after the Sun.
Tail of Comet Hyakutake 360 Reported for reference
IRC +10420 357[76]–1,342[27] L/Teff A yellow hypergiant that has increased its temperature into the LBV range.
The Pistol Star 340[77] Blue hypergiant, among the most massive and luminous stars known.
Mira A (Omicron Ceti) 332–402[78] AD Prototype Mira variable. De beck et al. 2010 calculates 541 R.[27]
La Superba (Y Canum Venaticorum) 307[27]–390[79] L/Teff Referred to as La Superba by Angelo Secchi. Currently one of the coolest and reddest stars.
Orbit of Mars 297–358 Reported for reference
Alpha Herculis (Ras Algethi) 284±60[80] The estimate ranges from 264 R to 303 R[80]
Sun's red giant phase 256[81] The core hydrogen would be exhausted in 5.4 billion years. In 7.9 billion years, The Sun would reach the tip of the red-giant branch of the Hertzsprung–Russell diagram. (see below)
Reported for reference
Orbit of Earth 215 (211–219) Reported for reference
Deneb (Alpha Cygni) 203±17[82] Prototype Alpha Cygni variable.
Solar System Habitable Zone 200–520[83] (uncertain) Reported for reference
Orbit of Venus 154–157 Reported for reference
Epsilon Aurigae A (Almaaz) 143–358[84] ε Aur was incorrectly claimed in 1970 as the largest star with a size between 2,000 R and 3,000 R,[85] even though it later turned out not to be an infrared light star but rather a dusk torus surrounding the system.
S Doradus 100–380[86] Prototype S Doradus variable, even though P Cygni was the first discovered.
Peony Star 92[87] Candidate for most luminous star in the Milky Way.
Rigel A (Beta Orionis A) 78.9[88]–115[89] Margin of possible error: ±7.4 R.[88]
Canopus (Alpha Carinae) 71±4[90] Second brightest star in the night sky.
Orbit of Mercury 66–100 Reported for reference
LBV 1806-20 45–145[91] L/Teff Formerly a candidate for the most luminous star in the Milky Way with 40 million L,[92] but the luminosity has been revised later only 2–5 million L.[93][94]
Aldebaran (Alpha Tauri) 44.13±0.84[95] AD
Polaris (Alpha Ursae Minoris) 37.5[96] The current northern pole star.
R136a1 28.8[97]–35.4[98] Also on record as the most massive and luminous star known (265 - 315 M and 8.71 million L).
Arcturus (Alpha Boötis) 25.4±0.2[99] Brightest star in the northern hemisphere.
HDE 226868 20–22[100] The supergiant companion of black hole Cygnus X-1. The black hole is 500,000 times smaller than the star.
VV Cephei B 13[101]–25[102] The B-type main sequence companion of VV Cephei A.
Sun's helium burning phase 10 After the red-giant branch the Sun has approximately 120 million years of active life left.
Reported for reference
Sun 1 The largest object in the Solar System.
Reported for reference
  1. ^ AD: radius determined from angular diameter and distance
    L/Teff: radius calculated from bolometric luminosity and effective temperature

See also

References

  1. ^ a b c d e f g h i j k l m n o p q r s t u v w x y Table 4 in Levesque, Emily M.; Massey, Philip; Olsen, K. A. G.; Plez, Bertrand; Josselin, Eric; Maeder, Andre; Meynet, Georges (2005). "The Effective Temperature Scale of Galactic Red Supergiants: Cool, but Not as Cool as We Thought". The Astrophysical Journal. 628 (2): 973–985. arXiv:astro-ph/0504337. Bibcode:2005ApJ...628..973L. doi:10.1086/430901.
  2. ^ a b c d e f g h i j k l m n o p q r s t u v w x y z aa ab ac ad ae af ag ah ai aj ak al am an ao ap aq ar as at Levesque, Emily M.; Massey, Philip; Olsen, K.A.G.; Plez, Bertrand; Meynet, Georges; Maeder, Andre (2006). "The Effective Temperatures and Physical Properties of Magellanic Cloud Red Supergiants: The Effects of Metallicity". The Astrophysical Journal. 645 (2): 1102–1117. arXiv:astro-ph/0603596. Bibcode:2006ApJ...645.1102L. doi:10.1086/504417.
  3. ^ a b c d Arroyo-Torres, B; Wittkowski, M; Marcaide, J. M; Hauschildt, P. H (June 2013). "The atmospheric structure and fundamental parameters of the red supergiants AH Scorpii, UY Scuti, and KW Sagittarii". Astronomy & Astrophysics. 554 (A76): A76. arXiv:1305.6179. Bibcode:2013A&A...554A..76A. doi:10.1051/0004-6361/201220920.
  4. ^ Levesque, Emily M; Massey, Philip; Plez, Bertrand; Olsen, Knut A. G (June 2009). "The Physical Properties of the Red Supergiant WOH G64: The Largest Star Known?". Astronomical Journal. 137 (6): 4744. arXiv:0903.2260. Bibcode:2009AJ....137.4744L. doi:10.1088/0004-6256/137/6/4744.
  5. ^ Ohnaka, K.; Driebe, T.; Hofmann, K. H.; Weigelt, G.; Wittkowski, M. (2009). "Resolving the dusty torus and the mystery surrounding LMC red supergiant WOH G64". Proceedings of the International Astronomical Union. 4: 454. Bibcode:2009IAUS..256..454O. doi:10.1017/S1743921308028858.
  6. ^ Humphreys, R. M. (1978). "Studies of luminous stars in nearby galaxies. I. Supergiants and O stars in the Milky Way". The Astrophysical Journal Supplement Series. 38: 309. Bibcode:1978ApJS...38..309H. doi:10.1086/190559.
  7. ^ Davies, Ben; Kudritzki, Rolf-Peter; Figer, Donald F. (2010). "The potential of red supergiants as extragalactic abundance probes at low spectral resolution". Monthly Notices of the Royal Astronomical Society. 407 (2): 1203. arXiv:1005.1008. Bibcode:2010MNRAS.407.1203D. doi:10.1111/j.1365-2966.2010.16965.x.
  8. ^ Wright, Nicholas J; Wesson, Roger; Drew, Janet E; Barentsen, Geert; Barlow, Michael J; Walsh, Jeremy R; Zijlstra, Albert; Drake, Jeremy J; Eislöffel, Jochen; Farnhill, Hywel J (2014). "The ionized nebula surrounding the red supergiant W26 in Westerlund 1". Monthly Notices of the Royal Astronomical Society: Letters. 437 (1): L1. arXiv:1309.4086. Bibcode:2014MNRAS.437L...1W. doi:10.1093/mnrasl/slt127.
  9. ^ a b c d e f g h i j k Fok, Thomas K. T; Nakashima, Jun-ichi; Yung, Bosco H. K; Hsia, Chih-Hao; Deguchi, Shuji (2012). "Maser Observations of Westerlund 1 and Comprehensive Considerations on Maser Properties of Red Supergiants Associated with Massive Clusters". The Astrophysical Journal. 760: 65. arXiv:1209.6427. doi:10.1088/0004-637X/760/1/65.
  10. ^ Blum, R. D; Ramirez, Solange V; Sellgren, K; Olsen, K (2003). "Really Cool Stars and the Star Formation History at the Galactic Center". The Astrophysical Journal. 597: 323–346. doi:10.1086/378380.
  11. ^ Moffat, A. F. J. (August 1976). "Mass loss from the M 3 supergiant HD 143183 in a young compact star cluster in Norma". Astronomy and Astrophysics. 50 (3): 429–434. Bibcode:1976A&A....50..429M.
  12. ^ Wittkowski, M.; Hauschildt, P. H.; Arroyo-Torres, B.; Marcaide, J. M. (2012). "Fundamental properties and atmospheric structure of the red supergiant VY Canis Majoris based on VLTI/AMBER spectro-interferometry". Astronomy & Astrophysics. 540: L12. arXiv:1203.5194. Bibcode:2012A&A...540L..12W. doi:10.1051/0004-6361/201219126.
  13. ^ Choi, Yoon Kyung; et al. (2008). "Distance to VY CMa with VERA". Publications of the Astronomical Society of Japan. 60 (5): 1007. arXiv:0808.0641. Bibcode:2008PASJ...60.1007C. doi:10.1093/pasj/60.5.1007.
  14. ^ Alcolea, J; Bujarrabal, V; Planesas, P; Teyssier, D; Cernicharo, J; De Beck, E; Decin, L; Dominik, C; Justtanont, K; De Koter, A; Marston, A. P; Melnick, G; Menten, K. M; Neufeld, D. A; Olofsson, H; Schmidt, M; Schöier, F. L; Szczerba, R; Waters, L. B. F. M (2013). "HIFISTARSHerschel/HIFI observations of VY Canis Majoris". Astronomy & Astrophysics. 559: A93. doi:10.1051/0004-6361/201321683.
  15. ^ a b c d e f g h i j k l m Davies, B.; Figer, D. F.; Law, C. J.; Kudritzki, R. P.; Najarro, F.; Herrero, A.; MacKenty, J. W. (2008). "The Cool Supergiant Population of the Massive Young Star Cluster RSGC1". The Astrophysical Journal. 676 (2): 1016–1028. arXiv:0711.4757. Bibcode:2008ApJ...676.1016D. doi:10.1086/527350.
  16. ^ a b c d e f g h i j k l Marshall, Jonathan R; van Loon, Jacco Th; Matsuura, Mikako; Wood, Peter R; Zijlstra, Albert A; Whitelock, Patricia A (2004). "The AGB superwind speed at low metallicity". Monthly Notices of the Royal Astronomical Society. 355 (4): 1348. arXiv:astro-ph/0410120. doi:10.1111/j.1365-2966.2004.08417.x.
  17. ^ Chesneau, O.; Meilland, A.; Chapellier, E.; Millour, F.; Van Genderen, A. M.; Nazé, Y.; Smith, N.; Spang, A.; Smoker, J. V.; Dessart, L.; Kanaan, S.; Bendjoya, Ph.; Feast, M. W.; Groh, J. H.; Lobel, A.; Nardetto, N.; Otero, S.; Oudmaijer, R. D.; Tekola, A. G.; Whitelock, P. A.; Arcos, C.; Curé, M.; Vanzi, L. (2014). "The yellow hypergiant HR 5171 A: Resolving a massive interacting binary in the common envelope phase". Astronomy & Astrophysics. 563: A71. arXiv:1401.2628v2. Bibcode:2014A&A...563A..71C. doi:10.1051/0004-6361/201322421.
  18. ^ a b 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. (October 2017) [Published online: 29 September 2017]. "Multi-epoch VLTI-PIONIER imaging of the supergiant V766 Cen: Image of the close companion in front of the primary". Astronomy & Astrophysics. 606 (1): L1. arXiv:1709.09430. Bibcode:2017arXiv170909430W. doi:10.1051/0004-6361/201731569.
  19. ^ 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". Astronomy & Astrophysics. 597 (9): A9. arXiv:1610.01927. Bibcode:2017A&A...597A...9W. doi:10.1051/0004-6361/201629349.
  20. ^ Levesque, Emily M; Massey, Philip; Olsen, K. A. G; Plez, Bertrand; Meynet, George; Maeder, Andre; Boyer, Martha; Decin, L; Khouri, Theo; Meixner, Margaret; Van Loon, Jacco Th; Woods, Paul M (2016). "The mass-loss rates of red supergiants at low metallicity: Detection of rotational CO emission from two red supergiants in the Large Magellanic Cloud". Monthly Notices of the Royal Astronomical Society. 462 (3): 2995–3005. arXiv:1608.01729. doi:10.1093/mnras/stw1853.
  21. ^ 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. arXiv:0705.0266. Bibcode:2007A&A...469..671J. doi:10.1051/0004-6361:20066353.
  22. ^ a b Ahad, Abdul (May 1, 2004). "The second 'Garnet Star' after Mu Cephei must be 119 Tauri!". Google Groups.
  23. ^ 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. arXiv:astro-ph/0008058. Bibcode:2000ApJ...540L..99T. doi:10.1086/312879.
  24. ^ 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.
  25. ^ 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 (1): 843. arXiv:1310.2245. Bibcode:2014MNRAS.437..843G. doi:10.1093/mnras/stt1943.
  26. ^ 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.
  27. ^ a b c d e f g h i De Beck, E.; Decin, L.; De Koter, A.; Justtanont, K.; Verhoelst, T.; Kemper, F.; Menten, K. M. (2010). "Probing the mass-loss history of AGB and red supergiant stars from CO rotational line profiles. II. CO line survey of evolved stars: Derivation of mass-loss rate formulae". Astronomy and Astrophysics. 523: A18. arXiv:1008.1083. Bibcode:2010A&A...523A..18D. doi:10.1051/0004-6361/200913771.
  28. ^ 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: 273–289. arXiv:astro-ph/0504379. Bibcode:2005A&A...438..273V. doi:10.1051/0004-6361:20042555.
  29. ^ De Jager, C; Nieuwenhuijzen, H; Van Der Hucht, K. A (1988). "Mass loss rates in the Hertzsprung-Russell diagram". Astronomy and Astrophysics Supplement Series. 72: 259. Bibcode:1988A&AS...72..259D. ISSN 0365-0138.
  30. ^ 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.
  31. ^ Beasor, Emma R; Davies, Ben; 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 (2018). "The evolution of red supergiant mass-loss rates". Monthly Notices of the Royal Astronomical Society. 475 (1): 55. Bibcode:2018MNRAS.475...55B.
  32. ^ Xu, Shuangjing; Zhang, Bo; Reid, Mark J; Menten, Karl M; Zheng, Xingwu; Wang, Guangli (2018). "The Parallax of the Red Hypergiant VX Sgr with Accurate Tropospheric Delay Calibration". The Astrophysical Journal. 859 (1): 14. arXiv:1804.00894. Bibcode:2018ApJ...859...14X. doi:10.3847/1538-4357/aabba6.
  33. ^ 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.
  34. ^ 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 (1): 301–310. arXiv:astro-ph/0701769. Bibcode:2007ApJ...660..301M. doi:10.1086/513182.
  35. ^ 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.
  36. ^ a b c Mauron, N.; Josselin, E. (2011). "The mass-loss rates of red supergiants and the de Jager prescription". Astronomy and Astrophysics. 526: A156. arXiv:1010.5369. Bibcode:2011A&A...526A.156M. doi:10.1051/0004-6361/201013993.
  37. ^ Verhoelst, T.; Van Der Zypen, N.; Hony, S.; Decin, L.; Cami, J.; Eriksson, K. (2009). "The dust condensation sequence in red supergiant stars". Astronomy and Astrophysics. 498: 127–138. arXiv:0901.1262. Bibcode:2009A&A...498..127V. doi:10.1051/0004-6361/20079063.
  38. ^ Levesque, Emily M; Massey, Philip; Olsen, K. A. G; Plez, Bertrand; Meynet, George; Maeder, Andre (2018). "The Dusty Progenitor Star of the Type II Supernova 2017eaw". arXiv:1806.00348 [astro-ph.SR].
  39. ^ a b Paumard, T; Pfuhl, O; Martins, F; Kervella, P; Ott, T; Pott, J-U; Le Bouquin, JB; Breitfelder, J; Gillessen, S; Perrin, G; Burtscher, L; Haubois, X; Brandner, W (2014). "GCIRS 7, a pulsating M1 supergiant at the Galactic centre . Physical properties and age". Astronomy & Astrophysics. 568 (85): A85. arXiv:1406.5320. Bibcode:2014A&A...568A..85P. doi:10.1051/0004-6361/201423991.
  40. ^ a b Pott, J.-U.; Eckart, A.; Glindemann, A.; Kraus, S.; Schöde, R.; Ghez, A. M.; Woillez, J.; Weigelt, G. (2008). "First VLTI infrared spectro-interferometry on GCIRS 7". Astronomy & Astrophysics. 487: 413–418. doi:10.1051/0004-6361/201423991.
  41. ^ 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.
  42. ^ 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 (1): 7. arXiv:1406.3143v2. Bibcode:2016ApJ...819....7D. doi:10.3847/0004-637X/819/1/7.
  43. ^ Lang, Kenneth R (2013-05-24). Essential Astrophysics. ISBN 9783642359637.
  44. ^ a b c d e f g Massey, Philip; Silva, David R; Levesque, Emily M; Plez, Bertrand; Olsen, Knut A. G; Clayton, Geoffrey C; Meynet, Georges; Maeder, Andre (2009). "Red Supergiants in the Andromeda Galaxy (M31)". The Astrophysical Journal. 703: 420–440. arXiv:0907.3767. doi:10.1088/0004-637X/703/1/420.
  45. ^ 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. arXiv:0903.1672. Bibcode:2009A&A...499..515R. doi:10.1051/0004-6361/200911730.
  46. ^ 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. arXiv:astro-ph/0605664. Bibcode:2006A&A...454L.103R. doi:10.1051/0004-6361:20065285.
  47. ^ 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–L98. arXiv:1406.0001. Bibcode:2014MNRAS.443L..94L. doi:10.1093/mnrasl/slu080.
  48. ^ Garcia-Hernandez, D. A; Manchado, A; Lambert, D. L; Plez, B; Garcia-Lario, P; D'Antona, F; Lugaro, M; Karakas, A. I; van Raai, M (2009). "Rb-rich Asymptotic Giant Branch stars in the Magellanic Clouds". The Astrophysical Journal. 705: L31–L35. arXiv:0909.4391. doi:10.1088/0004-637X/705/1/L31.
  49. ^ a b 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 (50): A50. arXiv:1501.01560. Bibcode:2015A&A...575A..50A. doi:10.1051/0004-6361/201425212.
  50. ^ Gull, T. R.; Damineli, A. (2010). "JD13 – Eta Carinae in the Context of the Most Massive Stars". Proceedings of the International Astronomical Union. 5: 373–398. arXiv:0910.3158. Bibcode:2010HiA....15..373G. doi:10.1017/S1743921310009890.
  51. ^ Smith, Nathan (2011). "Explosions triggered by violent binary-star collisions: Application to Eta Carinae and other eruptive transients". Monthly Notices of the Royal Astronomical Society. 415 (3): 2020–2024. arXiv:1010.3770. Bibcode:2011MNRAS.415.2020S. doi:10.1111/j.1365-2966.2011.18607.x.
  52. ^ a b 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 (1): 46. arXiv:1405.4032. Bibcode:2014ApJ...785...46B. doi:10.1088/0004-637X/785/1/46.
  53. ^ Stickland, D. J. (1985). "IRAS observations of the cool galactic hypergiants". The Observatory. 105: 229. Bibcode:1985Obs...105..229S.
  54. ^ Odenwald, S. F. (1986). "An IRAS survey of IR excesses in G-type stars". Astrophysical Journal. 307: 711. Bibcode:1986ApJ...307..711O. doi:10.1086/164456.
  55. ^ Richichi, A.; Percheron, I.; Khristoforova, M. (2005). "CHARM2: An updated Catalog of High Angular Resolution Measurements". Astronomy and Astrophysics. 431 (4): 773–777.
  56. ^ "Carina Constellation". Constellation Guide. Retrieved 2017-10-28.
  57. ^ 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.
  58. ^ Bergeat, J.; Chevallier, L. (2005). "The mass loss of C-rich giants". Astronomy and Astrophysics. 429 (2005): 235–246. arXiv:astro-ph/0601366. Bibcode:2005A&A...429..235B. doi:10.1051/0004-6361:20041280.
  59. ^ 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.
  60. ^ 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. 452: 314. Bibcode:1995ApJ...452..314H. doi:10.1086/176303.
  61. ^ Massey, Philip; Evans, Kate Anne (2016). "The Red Supergiant Content of M31". The Astrophysical Journal. 826 (2): 224. doi:10.3847/0004-637X/826/2/224.
  62. ^ a b 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.
  63. ^ Pugh, T.; Gray, D. F. (2013-02-01). "On the Six-year Period in the Radial Velocity of Antares A". The Astronomical Journal. 145 (2): 38. Bibcode:2013AJ....145...38P. doi:10.1088/0004-6256/145/2/38. ISSN 0004-6256.
  64. ^ Baade, R.; Reimers, D. (2007-10-01). "Multi-component absorption lines in the HST spectra of alpha Scorpii B". Astronomy and Astrophysics. 474: 229–237. Bibcode:2007A&A...474..229B. doi:10.1051/0004-6361:20077308. ISSN 0004-6361.
  65. ^ Montargès, M.; Norris, R.; Chiavassa, A.; Tessore, B.; Lèbre, A.; Baron, F. (June 2018). "The convective photosphere of the red supergiant CE Tau. I. VLTI/PIONIER H-band interferometric imaging". Astronomy & Astrophysics. 614 (12): A12. arXiv:1802.06086. doi:10.1051/0004-6361/201731471.
  66. ^ Parker, Greg (July 2, 2012). "The second reddest star in the sky – 119 Tauri, CE Tauri". New Forest Observatory.
  67. ^ a b Men'shchikov1, A. B.; Balega, Y.; Blöcker, T.; Osterbart, R.; Weigelt, G. (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. 392 (3): 921–929. arXiv:astro-ph/0206410. Bibcode:2002A&A...392..921M. doi:10.1051/0004-6361:20020954.
  68. ^ Weigelt, G.; et al. (May 1998). "76mas speckle-masking interferometry of IRC+10216 with the SAO 6m telescope: Evidence for a clumpy shell structure". Astronomy and Astrophysics. 333 (1998): L51–L54. arXiv:astro-ph/9805022. Bibcode:1998A&A...333L..51W.
  69. ^ 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.
  70. ^ a b 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.
  71. ^ Kaler, James B. "Hind's Crimson Star". STARS. Retrieved 2018-03-19.
  72. ^ 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.
  73. ^ Tylenda, R.; Kamiński, T.; Schmidt, M.; Kurtev, R.; Tomov, T. (2011). "High-resolution optical spectroscopy of V838 Monocerotis in 2009". Astronomy & Astrophysics. 532: A138. arXiv:1103.1763. Bibcode:2011A&A...532A.138T. doi:10.1051/0004-6361/201116858.
  74. ^ Lane, B. F.; Retter, A.; Thompson, R. R.; Eisner, J. A. (April 2005). "Interferometric Observations of V838 Monocerotis". The Astrophysical Journal. 622 (2): L137–L140. arXiv:astro-ph/0502293. Bibcode:2005ApJ...622L.137L. doi:10.1086/429619.
  75. ^ Bedding, T. R.; et al. (April 1997), "The angular diameter of R Doradus: a nearby Mira-like star", Monthly Notices of the Royal Astronomical Society, 286 (4): 957–962, arXiv:astro-ph/9701021, Bibcode:1997MNRAS.286..957B, doi:10.1093/mnras/286.4.957
  76. ^ Dinh-V.-Trung; Muller, Sébastien; Lim, Jeremy; Kwok, Sun; Muthu, C. (2009). "Probing the Mass-Loss History of the Yellow Hypergiant IRC+10420". The Astrophysical Journal. 697 (1): 409–419. arXiv:0903.3714v1. Bibcode:2009ApJ...697..409D. doi:10.1088/0004-637X/697/1/409.
  77. ^ Najarro, F.; Figer, D. F.; Hillier, D. J.; Geballe, T. R.; Kudritzki, R. P. (2009). "Metallicity in the Galactic Center: The Quintuplet Cluster". The Astrophysical Journal. 691 (2): 1816–1827. arXiv:0809.3185. Bibcode:2009ApJ...691.1816N. doi:10.1088/0004-637X/691/2/1816.
  78. ^ Woodruff, H. C.; Eberhardt, M.; Driebe, T.; Hofmann, K.-H.; et al. (2004). "Interferometric observations of the Mira star o Ceti with the VLTI/VINCI instrument in the near-infrared". Astronomy & Astrophysics. 421 (2): 703–714. arXiv:astro-ph/0404248. Bibcode:2004A&A...421..703W. doi:10.1051/0004-6361:20035826.
  79. ^ 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.
  80. ^ a b 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.
  81. ^ Rybicki, K. R.; Denis, C. (2001). "On the Final Destiny of the Earth and the Solar System". Icarus. 151 (1): 130–137. Bibcode:2001Icar..151..130R. doi:10.1006/icar.2001.6591.
  82. ^ Schiller, F.; Przybilla, N. (2008). "Quantitative spectroscopy of Deneb". Astronomy & Astrophysics. 479 (3): 849–858. arXiv:0712.0040. Bibcode:2008A&A...479..849S. doi:10.1051/0004-6361:20078590.
  83. ^ Ramirez, Ramses; Kaltenegger, Lisa (2017). "A Volcanic Hydrogen Habitable Zone". The Astrophysical Journal Letters. 837 (1): L4. arXiv:1702.08618 [astro-ph.EP]. Bibcode:2017ApJ...837L...4R. doi:10.3847/2041-8213/aa60c8. Cite uses deprecated parameter |class= (help)
  84. ^ Kloppenborg, B.K.; Stencel, R.E.; Monnier, J.D.; Schaefer, G.H.; Baron, F.; Tycner, C.; Zavala, R.T.; Hutter, D.; Zhao, M.; Che, X.; Ten Brummelaar, T.A.; Farrington, C.D.; Parks, R.; McAlister, H. A.; Sturmann, J.; Sturmann, L.; Sallave-Goldfinger, P.J.; Turner, N.; Pedretti, E.; Thureau, N. (2015). "Interferometry of ɛ Aurigae: Characterization of the Asymmetric Eclipsing Disk". The Astrophysical Journal Supplement Series. 220 (1): 14. arXiv:1508.01909. Bibcode:2015ApJS..220...14K. doi:10.1088/0067-0049/220/1/14.
  85. ^ "Ask Andy: The Biggest Star". Ottawa Citizen. Nov 27, 1970. p. 23.
  86. ^ Lamers, H. J. G. L. M. (February 6–10, 1995). "Observations and Interpretation of Luminous Blue Variables". Proceedings of IAU Colloquium 155, Astrophysical applications of stellar pulsation. Astrophysical applications of stellar pulsation. Astronomical Society of the Pacific Conference Series. 83. Cape Town, South Africa: Astronomical Society of the Pacific. pp. 176–191. Bibcode:1995ASPC...83..176L.
  87. ^ Barniske, A.; Oskinova, L. M.; Hamann, W. -R. (2008). "Two extremely luminous WN stars in the Galactic center with circumstellar emission from dust and gas". Astronomy and Astrophysics. 486 (3): 971. arXiv:0807.2476. Bibcode:2008A&A...486..971B. doi:10.1051/0004-6361:200809568.
  88. ^ a b 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.
  89. ^ 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.
  90. ^ 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.
  91. ^ Eikenberry, S. S.; Matthews, K.; Lavine, J. L.; Garske, M. A.; Hu, D.; Jackson, M. A.; Patel, S. G.; Barry, D. J.; Colonno, M. R.; Houck, J. R.; Wilson, J. C.; Corbel, S.; Smith, J. D. (2004). "Infrared Observations of the Candidate LBV 1806‐20 and Nearby Cluster Stars". The Astrophysical Journal. 616 (1): 506–518. arXiv:astro-ph/0404435. Bibcode:2004ApJ...616..506E. doi:10.1086/422180.
  92. ^ Kennedy, Meghan. "LBV 1806-20 AB?". SolStation.com.
  93. ^ Figer, D. F.; Najarro, F.; Kudritzki, R. P. (2004). "The Double-lined Spectrum of LBV 1806-20". The Astrophysical Journal. 610 (2): L109–L112. arXiv:astro-ph/0406316. Bibcode:2004ApJ...610L.109F. doi:10.1086/423306.
  94. ^ Nazé, Y.; Rauw, G.; Hutsemékers, D. (2012). "The first X-ray survey of Galactic luminous blue variables". Astronomy & Astrophysics. 538 (47): A47. arXiv:1111.6375. Bibcode:2012A&A...538A..47N. doi:10.1051/0004-6361/201118040.
  95. ^ Piau, L; Kervella, P; Dib, S; Hauschildt, P (February 2011). "Surface convection and red-giant radius measurements". Astronomy and Astrophysics. 526: A100. arXiv:1010.3649. Bibcode:2011A&A...526A.100P. doi:10.1051/0004-6361/201014442.
  96. ^ Fadeyev, Y. A. (2015). "Evolutionary status of Polaris". Monthly Notices of the Royal Astronomical Society. 449 (1): 1011–1017. arXiv:1502.06463. Bibcode:2015MNRAS.449.1011F. doi:10.1093/mnras/stv412.
  97. ^ Hainich, R.; Rühling, U.; Todt, H.; Oskinova, L. M.; Liermann, A.; Gräfener, G.; Foellmi, C.; Schnurr, O.; Hamann, W. -R. (2014). "The Wolf–Rayet stars in the Large Magellanic Cloud". Astronomy & Astrophysics. 565 (27): A27. arXiv:1401.5474. Bibcode:2014A&A...565A..27H. doi:10.1051/0004-6361/201322696.
  98. ^ 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): 731–751. arXiv:1007.3284. Bibcode:2010MNRAS.408..731C. doi:10.1111/j.1365-2966.2010.17167.x.
  99. ^ Ramírez, I.; Allende Prieto, C. (December 2011). "Fundamental Parameters and Chemical Composition of Arcturus". The Astrophysical Journal. 743 (2): 135. arXiv:1109.4425. Bibcode:2011ApJ...743..135R. doi:10.1088/0004-637X/743/2/135.
  100. ^ 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, see Table 1 with d=2 kpc.
  101. ^ 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.
  102. ^ 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. 95: 589. Bibcode:1992A&AS...95..589H. ISSN 0365-0138.

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