List of hottest stars

Last updated

This is a list of hottest stars so far discovered (excluding degenerate stars), arranged by decreasing temperature. The stars with temperatures higher than 60,000 K are included.

Contents

List

Star nameEffective
Temperature
(K)		Mass
(M☉)		Luminosity
(L☉)		 Spectral type Distance
(light-years)		Ref.
WR 102 200,00016.1380,000 WO2 8,610 [1] [2] [3]
WR 142 200,00028.6912,000 WO2 5,400 [3]
LMC195-1 200,000257,000 WO2 ~160,000 [4]
BAT99-123 170,0007.7158,000 WO3 ~160,000 [5]
WR 93b 160,0008.1110,000 WO3 7,470 [1] [3]
[HC2007] 31160,000? WO3 12,886,000 [6]
BAT99-53 A 158,00013224,000 WC4 ~160,000 [7]
BAT99-7 158,00025692,000 WN4b ~160,000 [8]
IC 1613 DR1150,00020480,000 WO3 ~2,380,000 [9]
LH41-1042 150,0008.4182,000 WO4 ~160,000 [5]
BAT99-2 141,00013234,000 WN2 ~160,000 [8]
BAT99-94 141,00024631,000 WN3 ~160,000 [8]
WR 2 141,00016282,000 WN2 7,830 [1]
AB8 141,000191,413,000 WO4 ~197,000 [5]
BA 1-458 140,00028.1776,000 WO4 2,500,000 [10]
WR 9 (WR)139,7009501,000 WC4 14,900 [1]
WR 30a (WR)129,5007.5-9.7195,000 WO4 25,340 [11]
WR 38 126,00010.4724,000 [12] WC4 19,700 [12] [3]
WR 142a 125,0007.9110,000 WC8 5,900 [12] [13]
BAT99-128 112,00014275,000 WN3 ~160,000 [8]
WR 1 112,00027759,000 WN4-s 10,300 [1] [14]
WR 18 112,000381,288,000 WN4-s 12,500 [1] [14]
WR 46 112,00014263,000 WN3pw 13,000
WR 7 112,00013214,000 WN4-s 14,000 [14]
WR 144 112,0009.9159,000 WC4 5,710 [1] [3]
WR 52112,0008.5117,000 WC4 5,710 [1] [3]
AB7 105,000231,259,000 WN4 ~197,000 [15]
BAT99-24 100,00017347,000 WN4b ~160,000 [8]
WR 37 100,000341,122,000 WN4-s 21,900 [12]
NGC 6822-WR 12 100,000361,288,000 WN4 ~1,631,000 [10]
Gamma Velorum (WR)90,0009204,000 WC8 1,100 [16]
BAT99-1 89,10012200,000 WN3b ~160,000 [8]
EZ CMa 89,10023617,000 WN4-s 5,900[ citation needed ] [17]
WR 36 89,10012200,000 WN5-s 17,700 [1] [14]
WR 111 89,10013245,000 WC5 5,320 [1] [3]
WR 150 89,10024.8724,000 WC5 28,500 [1] [3]
BAT99-3 79,40016324,000 WN4b ~160,000 [8]
WR 19 A 79,400400,000 WC5d 14,000 [1] [18] [19]
WR 44 79,40018417,000 WN4-w 19,800 [1] [14]
WR 58 79,4008.489,100 WN4/WCE 19,700 [1] [3]
BAT99-37 79,40019447,000 WN3o 160,000 [8]
WR 45 79,40014.1282,000 WC6 13,900 [1] [3]
BAT99-26 70,80018417,000 WN4b ~160,000 [8]
BAT99-35 70,80024398,000 WN3(h) ~160,000 [8]
BAT99-86 70,80012427,000 WN3(h) ~160,000 [8]
WR 136 70,80015260,000 WN6(h)-s 6,290 [1]
WR 75 63,10018389,000 WN6-s 10,800 [1] [14]
WR 134 63,10019400,000 WN6-s 6,000 [14]
WR 60 63,10023631,000 WC8 11,500 [1] [3]
WR 149 63,10014269,000 WN5-s 15,900 [1] [14]

See also

Related Research Articles

<span class="mw-page-title-main">R136b</span> Star in the constellation Dorado

R136b is a blue supergiant star in the R136 cluster in the Large Magellanic Cloud. It is one of the most massive and most luminous stars known. It is found in the dense R136 open cluster at the centre of NGC 2070 in the Tarantula Nebula.

<span class="mw-page-title-main">WR 102ka</span> Star in the constellation Sagittarius

WR 102ka, also known as the Peony star, is a slash star that is one of several candidates for the most luminous-known star in the Milky Way.

<span class="mw-page-title-main">WR 102ea</span> Star in the constellation Sagittarius

WR 102ea is a Wolf–Rayet star in the Sagittarius constellation. It is the third most luminous star in the Quintuplet cluster after WR 102hb. With a luminosity of 2,500,000 times solar, it is also one of the most luminous stars known. Despite the high luminosity it can only be observed at infra-red wavelengths due to the dimming effect of intervening dust on visual light.

<span class="mw-page-title-main">NGC 371</span> Open cluster in the constellation Tucana

NGC 371, also called Hodge 53, is an open cluster 200,000 light-years away located in the Small Magellanic Cloud in Tucana constellation. It was discovered on 1 August 1826 by Scottish astronomer James Dunlop.

<span class="mw-page-title-main">Melnick 42</span> Massive blue supergiant star in the constellation Dorado

Melnick 42 is a massive blue supergiant star in the Tarantula Nebula in the Large Magellanic Cloud located in the constellation Dorado. Although it is only 21 times the size of the sun, its high temperature of 47,300 K makes it one of the most luminous stars of the Tarantula Nebula at 3,600,000 L☉. It is less than two parsecs from the centre of the R136 cluster, although that is well outside the central core.

HD 38282 is a massive spectroscopic binary star in the Tarantula Nebula, consisting of two hydrogen-rich Wolf-Rayet stars.

WR 142 is a Wolf-Rayet star in the constellation Cygnus, an extremely rare star on the WO oxygen sequence. It is a luminous and very hot star, highly evolved and close to exploding as a supernova. It is suspected to be a binary star with a companion orbiting about 1 AU away.

<span class="mw-page-title-main">Melnick 34</span> Binary star in the Large Magellanic cloud

Melnick 34, also called BAT99-116, is a binary Wolf–Rayet star near R136 in the 30 Doradus complex in the Large Magellanic Cloud. Both components are amongst the most massive and most luminous stars known, and the system is the most massive known binary system.

BAT99-98 is a Wolf–Rayet star located in the Large Magellanic Cloud, in NGC 2070 near the R136 cluster in the Tarantula Nebula. At 226 M☉ and 5,000,000 L☉ it is one of the most massive and luminous stars currently known.

<span class="mw-page-title-main">WR 102</span> Star in the constellation Sagittarius

WR 102 is a Wolf–Rayet star in the constellation Sagittarius, an extremely rare star on the WO oxygen sequence. It is a luminous and very hot star, highly evolved and close to exploding as a supernova.

WR 114 is a Wolf-Rayet star in the constellation of Scutum. It is an early type star of the carbon sequence (WCE) classified as WC5.

<span class="mw-page-title-main">WR 93b</span> Wolf-Rayet star in the constellation of Scorpius

WR 93b is a Wolf-Rayet star in the constellation Scorpius, an extremely rare star on the WO oxygen sequence. It appears near NGC 6357 in the tail of the scorpion.

WR 2 is a Wolf-Rayet star located around 8,000 light years away from Earth in the constellation of Cassiopeia, in the stellar association Cassiopeia OB1. It is smaller than the Sun, but due to a temperature over 140,000 K it is 282,000 times as luminous as the Sun. With a radius of 89% that of the Sun, it is the smallest known WN star in the Milky Way.

<span class="mw-page-title-main">WR 128</span> Wolf-Rayet star in the constellation Sagitta

WR 128 is a Wolf–Rayet star located about 9,500 light years away in the constellation of Sagitta. A member of the WN class, WR 128's spectrum resembles that of a WN4 star, but hydrogen is clearly present in the star, making it the only known hydrogen-rich WN4 star in the galaxy. However, similar H-rich very early WN stars can be found in the LMC and especially in the SMC, but the only other galactic examples of this are WR 3 and WR 152.

WR 69 is a Wolf–Rayet star located 11,350 light years away in the constellation of Triangulum Australe. It is classified as a WC9 star, belonging to the late-type carbon sequence. WR 69 is also a prolific dust maker, hence the "d" in its spectral type.

WR 150 is a Wolf-Rayet star in the constellation of Cygnus. It is one of the early-type carbon sequence (WCE), and is of spectral type WC5. WR 150 is very far from the Earth, being 28,500 light-years from it.

<span class="mw-page-title-main">WR 120</span> Binary star system in the constellation Scutum

WR 120 is a binary containing two Wolf-Rayet stars in the constellation of Scutum, around 10,000 light years away. The primary is a hydrogen-free weak-lined WN7 star, the secondary is a hydrogen-free WN3 or 4 star, and the system is a possible member of the cluster Dolidze 33. From our point of view, WR 120 is reddened by 4.82 magnitudes, and it has the variable designation of V462 Scuti.

BAT99-7 is a WN-type Wolf-Rayet star located in the Large Magellanic Cloud, in the constellation of Dorado, about 160,000 light years away. The star has a spectrum containing extremely broad emission lines, and is the prototype for the "round line" stars, Wolf-Rayet stars whose spectra are characterized by strong and broad emission lines with round line profiles. The broad emission lines hint at an extremely high temperature of nearly 160,000 Kelvin, which would make it the hottest of all WN stars with known temperatures, as well as an extraordinarily large mass loss rate for a Wolf-Rayet star in the LMC, at 10−4.48 M☉/yr, which means that every 30,200 years, the star loses 1 solar mass worth of mass.

WR 119 is a Wolf–Rayet star located about 10,500 light years away in the constellation Scutum. WR 119 is classified as a WC9 star, belonging to the late-type carbon sequence of Wolf-Rayet stars. WR 119 is noteworthy for being the least luminous known Wolf-Rayet star, at just over 50,000 L☉. The most recent estimate is even lower, at just 42,700 L☉, based on the most recent analysis using Gaia DR2 data.

References

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  2. ↑ Sander, A.; Hamann, W. -R.; Todt, H. (2012). "The Galactic WC stars". Astronomy & Astrophysics. 540: A144. arXiv: 1201.6354 . Bibcode:2012A&A...540A.144S. doi:10.1051/0004-6361/201117830. S2CID   119182468.
  3. 1 2 3 4 5 6 7 8 9 10 11 Sander, A. A. C.; Hamann, W.-R.; Todt, H.; Hainich, R.; Shenar, T.; Ramachandran, V.; Oskinova, L. M. (2019-01-01). "The Galactic WC and WO stars. The impact of revised distances from Gaia DR2 and their role as massive black hole progenitors". Astronomy and Astrophysics. 621: A92. arXiv: 1807.04293 . Bibcode:2019A&A...621A..92S. doi: 10.1051/0004-6361/201833712 . ISSN   0004-6361.
  4. ↑ Massey, Philip (2014). "A modern search for Wolf–Rayet stars in the Magellanic Clouds: First results". The Astrophysical Journal. 788 (1): 83. arXiv: 1404.7441 . Bibcode:2014ApJ...788...83M. doi:10.1088/0004-637X/788/1/83. S2CID   119177379.
  5. 1 2 3 Tramper, F.; Straal, S. M.; Sanyal, D.; Sana, H.; De Koter, A.; Gräfener, G.; Langer, N.; Vink, J. S.; De Mink, S. E.; Kaper, L. (2015). "Massive stars on the verge of exploding: The properties of oxygen sequence Wolf-Rayet stars". Astronomy & Astrophysics. 581: A110. arXiv: 1507.00839 . Bibcode:2015A&A...581A.110T. doi:10.1051/0004-6361/201425390. S2CID   56093231.
  6. ↑ Hadfield, L. J.; Crowther, P. A. (October 2007). "A survey of the Wolf-Rayet population of the barred, spiral galaxy NGC 1313". Monthly Notices of the Royal Astronomical Society. 381 (1): 418–432. arXiv: 0708.2039 . Bibcode:2007MNRAS.381..418H. doi: 10.1111/j.1365-2966.2007.12284.x . ISSN   0035-8711. S2CID   3024190.
  7. ↑ Ramachandran, V.; Hamann, W.-R.; Hainich, R.; Oskinova, L. M.; Shenar, T.; Sander, A. A. C.; Todt, H.; Gallagher, J. S. (2018-07-01). "Stellar population of the superbubble N 206 in the LMC. II. Parameters of the OB and WR stars, and the total massive star feedback". Astronomy and Astrophysics. 615: A40. arXiv: 1802.07494 . Bibcode:2018A&A...615A..40R. doi: 10.1051/0004-6361/201832816 . ISSN   0004-6361.
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  9. ↑ Tramper, F.; Gräfener, G.; Hartoog, O. E.; Sana, H.; De Koter, A.; Vink, J. S.; Ellerbroek, L. E.; Langer, N.; Garcia, M.; Kaper, L.; De Mink, S. E. (2013). "On the nature of WO stars: A quantitative analysis of the WO3 star DR1 in IC 1613". Astronomy & Astrophysics. 559: A72. arXiv: 1310.2849 . Bibcode:2013A&A...559A..72T. doi:10.1051/0004-6361/201322155. S2CID   216079684.
  10. 1 2 Abbott, Jay Brian (2004). "Quantitative spectroscopic studies of Wolf-Rayet stars in local group galaxies". Ph.D. Thesis. Bibcode:2004PhDT.......161A.
  11. ↑ Nugis, T.; Lamers, H. J. G. L. M. (2000). "Mass-loss rates of Wolf-Rayet stars as a function of stellar parameters". Astronomy and Astrophysics. 360: 227. Bibcode:2000A&A...360..227N.
  12. 1 2 3 4 Rate, Gemma; Crowther, Paul A. (2020-03-01). "Unlocking Galactic Wolf-Rayet stars with Gaia DR2 - I. Distances and absolute magnitudes". Monthly Notices of the Royal Astronomical Society. 493 (1): 1512–1529. arXiv: 1912.10125 . Bibcode:2020MNRAS.493.1512R. doi: 10.1093/mnras/stz3614 . ISSN   0035-8711.
  13. ↑ Pasquali, A.; Comerón, F.; Gredel, R.; Torra, J.; Figueras, F. (2002-12-01). "A new Wolf-Rayet star in Cygnus". Astronomy and Astrophysics. 396 (2): 533–538. arXiv: astro-ph/0210179 . Bibcode:2002A&A...396..533P. doi:10.1051/0004-6361:20021373. ISSN   0004-6361.
  14. 1 2 3 4 5 6 7 8 Hamann, W.-R.; Gräfener, G.; Liermann, A.; Hainich, R.; Sander, A. A. C.; Shenar, T.; Ramachandran, V.; Todt, H.; Oskinova, L. M. (2019-05-01). "The Galactic WN stars revisited. Impact of Gaia distances on fundamental stellar parameters". Astronomy and Astrophysics. 625: A57. arXiv: 1904.04687 . Bibcode:2019A&A...625A..57H. doi:10.1051/0004-6361/201834850. ISSN   0004-6361. S2CID   104292503.
  15. ↑ Shenar, T.; Hainich, R.; Todt, H.; Sander, A.; Hamann, W.-R.; Moffat, A. F. J.; Eldridge, J. J.; Pablo, H.; Oskinova, L. M.; Richardson, N. D. (2016). "Wolf-Rayet stars in the Small Magellanic Cloud: II. Analysis of the binaries". Astronomy & Astrophysics. 1604: A22. arXiv: 1604.01022 . Bibcode:2016A&A...591A..22S. doi:10.1051/0004-6361/201527916. S2CID   119255408.
  16. ↑ Crowther, Paul A.; Barlow, M. J.; Royer, P.; Hillier, D. J.; Bestenlehner, J. M.; Morris, P. W.; Wesson, R. (2024-02-01). "Oxygen abundance of γ Vel from [O III] 88 μm Herschel/PACS spectroscopy". Monthly Notices of the Royal Astronomical Society. 528 (2): 2026–2039. arXiv: 2310.15170 . Bibcode:2024MNRAS.528.2026C. doi: 10.1093/mnras/stae145 . ISSN   0035-8711.
  17. ↑ Sota, A.; Maíz Apellániz, J.; Morrell, N. I.; Barbá, R. H.; Walborn, N. R.; Gamen, R. C.; Arias, J. I.; Alfaro, E. J.; Oskinova, L. M. (2019). "The Galactic WN stars revisited. Impact of Gaia distances on fundamental stellar parameters". Astronomy & Astrophysics. A57: 625. arXiv: 1904.04687 . Bibcode:2019A&A...625A..57H. doi:10.1051/0004-6361/201834850. S2CID   104292503.
  18. ↑ Paul Crowther. "Galactic Wolf Rayet Catalogue" . Retrieved 2021-05-27.
  19. ↑ Lau, Ryan M.; Eldridge, J. J.; Hankins, Matthew J.; Lamberts, Astrid; Sakon, Itsuki; Williams, Peredur M. (2020-07-01). "Revisiting the Impact of Dust Production from Carbon-rich Wolf-Rayet Binaries". The Astrophysical Journal. 898 (1): 74. arXiv: 2006.08695 . Bibcode:2020ApJ...898...74L. doi: 10.3847/1538-4357/ab9cb5 . ISSN   0004-637X. S2CID   219708543.
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