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List of most massive stars

February 20, 2023

This article is about mass. For radius, see List of largest stars.

This is a list of the most massive stars that have been discovered, in solar masses (M☉).

Uncertainties and caveats

Most of the masses listed below are contested and, being the subject of current research, remain under review and subject to constant revision of their masses and other characteristics. Indeed, many of the masses listed in the table below are inferred from theory, using difficult measurements of the stars' temperatures and absolute brightnesses. All the masses listed below are uncertain: Both the theory and the measurements are pushing the limits of current knowledge and technology. Both theories and measurements could be incorrect. For example, VV Cephei could be between 25–40 M☉, or 100 M☉, depending on which property of the star is examined.

 
Artist's impression of disc of obscuring material around a massive star.

Complications with distance and obscuring clouds

Since massive stars are rare, astronomers must look very far from Earth to find them. All the listed stars are many thousands of light years away, which makes measurements difficult. In addition to being far away, many stars of such extreme mass are surrounded by clouds of outflowing gas created by extremely powerful stellar winds; the surrounding gas interferes with the already difficult-to-obtain measurements of stellar temperatures and brightnesses, which greatly complicates the issue of estimating internal chemical compositions and structures.[a] This obstruction leads to difficulties in calculating parameters.

 
Eta Carinae is the bright spot hidden in the double-lobed dust cloud. It is the most massive star that has a Bayer designation. It was only discovered to be (at least) two stars in the past few decades.

Both the obscuring clouds and the great distances make it difficult to judge whether the star is just a single supermassive object or, instead, a multiple star system. A number of the “stars” listed below may actually be two or more companions orbiting too closely to distinguish by our telescopes, each star being massive in itself but not necessarily “supermassive” to either be on this list, or near the top of it. Other combinations are possible – for example a supermassive star with one or more smaller companions or more than one giant star – but without being able to see inside the surrounding cloud, it is difficult to know the truth of the matter.

More globally, statistics on stellar populations seem to indicate that the upper mass limit is in the 100–200 solar mass range,[1] so all mass estimates exceeding this range are suspect.

Rare reliable estimates

Eclipsing binary stars are the only stars whose masses are estimated with some confidence. However note that almost all of the masses listed in the table below were inferred by indirect methods; only a few of the masses in the table were determined using eclipsing systems.

 
WR 25 is a binary star, whose orbit around its obscured companion provided a constraint on its mass.

Amongst the most reliable listed masses are those for the eclipsing binaries NGC 3603-A1, WR 21a, and WR 20a. Masses for all three were obtained from orbital measurements.[b] This involves measuring their radial velocities and also their light curves. The radial velocities only yield minimum values for the masses, depending on inclination, but light curves of eclipsing binaries provide the missing information: inclination of the orbit to our line of sight.

Relevance of stellar evolution

Some stars may once have been more massive than they are today. It is likely that many large stars have suffered significant mass loss (perhaps as much as several tens of solar masses). This mass may have been expelled by superwinds: high velocity winds that are driven by the hot photosphere into interstellar space. The process forms an enlarged extended envelope around the star that interacts with the nearby interstellar medium and infusing the region with elements heavier than hydrogen or helium.[c]

There are also – or rather were – stars that might have appeared on the list but no longer exist as stars, or are supernova impostors; today we see only their debris.[d] The masses of the precursor stars that fueled these destructive events can be estimated from the type of explosion and the energy released, but those masses are not listed here (see § Black holes below).

Mass limits

There are two related theoretical limits on how massive a star can possibly be: the accretion limit and the Eddington mass limit. The accretion limit is related to star formation: After about 120 M☉ have accreted in a protostar, the combined mass should have become hot enough for its heat to drive away any further incoming matter. In effect, the protostar reaches a point where it evaporates away material as fast as it collects new material. The Eddington limit is based on light pressure from the core of an already-formed star: As mass increases past ~150 M☉, the intensity of light radiated from a Population I star's core will become sufficient for the light-pressure pushing outward to exceed the gravitational force pulling inward, and the surface material of the star will be free to float away into space.

Accretion limits

Astronomers have long hypothesized that as a protostar grows to a size beyond 120 M☉, something drastic must happen.[2] Although the limit can be stretched for very early Population III stars, and although the exact value is uncertain, if any stars still exist above 150–200 M☉ they would challenge current theories of stellar evolution.

Studying the Arches Cluster, which is currently the densest known cluster of stars in our galaxy, astronomers have confirmed that no stars in that cluster exceed about 150 M☉.

 
The R136 cluster is an unusually dense collection of young, hot, blue stars.

Rare ultramassive stars that exceed this limit – for example in the R136 star cluster – might be explained by the following proposal: Some of the pairs of massive stars in close orbit in young, unstable multiple-star systems must occasionally collide and merge where certain unusual circumstances hold that make a collision possible.[3]

Eddington mass limit

Main article: Eddington luminosity

A limit on stellar mass arises because of light-pressure: For a sufficiently massive star the outward pressure of radiant energy generated by nuclear fusion in the star's core exceeds the inward pull of its own gravity. The lowest mass for which this effect is active is the Eddington limit.

Stars of greater mass have a higher rate of core energy generation, and heavier stars' luminosities increase far out of proportion to the increase in their masses. The Eddington limit is the point beyond which a star ought to push itself apart, or at least shed enough mass to reduce its internal energy generation to a lower, maintainable rate. The actual limit-point mass depends on how opaque the gas in the star is, and metal-rich Population I stars have lower mass limits than metal-poor Population II stars. Before their demise, the hypothetical metal-free Population III stars would have had the highest allowed mass, somewhere around 300 M☉.

In theory, a more massive star could not hold itself together because of the mass loss resulting from the outflow of stellar material. In practice the theoretical Eddington Limit must be modified for high luminosity stars and the empirical Humphreys–Davidson limit is used instead.[4]

List of the most massive stars

The following two lists show a few of the known stars, including the stars in open cluster, OB association and H II region. Despite their high luminosity, many of them are nevertheless too distant to be observed with the naked eye. Stars that are at least sometimes visible to the unaided eye have their apparent magnitude (6.5 or brighter) highlighted in blue.

The first list gives stars that are estimated to be 60 M☉ or larger; the majority of which are shown. The second list includes some notable stars which are below 60 M☉ for the purpose of comparison. The method used to determine each star's mass is included to give an idea of the data's uncertainty; note that the mass of binary stars can be determined far more accurately. The masses listed below are the stars' current (evolved) mass, not their initial (formation) mass.

Stars with 60 M☉ or greater
Star name Mass
(M☉, Sun = 1) 		Approx. distance
from Earth (ly) 		Apparent
visible magnitude 		Effective
temperature (K) 		Estimation
method 		Link Reference
Westerhout 49-2 (in Westerhout 49) 250 36,200 18.246 (J band) 35,500 Spectroscopy SIMBAD [5][6]
BAT99-98 (in Tarantula Nebula of LMC) 226 165,000 13.37 45,000 Spectroscopy SIMBAD [7][8]
R136a1 (in Tarantula Nebula of LMC) 196 163,000 12.23 46,000 Evolution SIMBAD [9][10]
Melnick 42 (in Tarantula Nebula of LMC) 189 163,000 12.78 47,300 Spectroscopy SIMBAD [11][8]
VFTS 1022 (in Tarantula Nebula of LMC) 178 164,000 13.47 42,200 Spectroscopy SIMBAD [11][8]
Westerhout 51-57 (in Westerhout 51) 160 20,000 16.66 (J band) 42,700 Evolution [12]
R136a3 (in Tarantula Nebula of LMC) 155 163,000 12.97 50,000 Evolution SIMBAD [9][10]
VFTS 682 (in Tarantula Nebula of LMC) 153 164,000 16.08 52,200 Spectroscopy SIMBAD [13][8]
HD 15558 A (in IC 1805 of Heart Nebula) 152 24,400 7.87 (combined) 39,500 Binary SIMBAD [14][15]
R136a2 (in Tarantula Nebula of LMC) 151 163,000 12.34 50,000 Evolution SIMBAD [9][10]
Westerhout 51-3 (in Westerhout 51) 148 20,000 17.79 (J band) 39,800 Evolution SIMBAD [12]
Melnick 34 A (in Tarantula Nebula of LMC) 147 163,000 13.09 (combined) 53,000 Binary SIMBAD [16][8]
VFTS 482 (in Tarantula Nebula of LMC) 145 164,000 12.95 42,200 Spectroscopy SIMBAD [11][8]
R136c (in Tarantula Nebula of LMC) 142 163,000 13.43 51,000 Evolution SIMBAD [17][8]
VFTS 1021 (in Tarantula Nebula of LMC) 141 164,000 13.35 39,800 Spectroscopy SIMBAD [11][8]
LH 10-3209 A (in NGC 1763 of LMC) 140 160,000 11.859 (combined) 42,500 Spectroscopy SIMBAD [18][19][e]
VFTS 506 (in Tarantula Nebula of LMC) 138 164,000 13.31 47,300 Spectroscopy SIMBAD [13][8]
Melnick 34 B (in Tarantula Nebula of LMC) 136 163,000 13.09 (combined) 53,000 Binary SIMBAD [16][8]
Westerhout 51d (in Westerhout 51) 135 20,000 15.11 (J band) 42,700 Evolution [12]
VFTS 545 (in Tarantula Nebula of LMC) 133 164,000 13.32 47,300 Spectroscopy SIMBAD [11][8]
HD 97950 B (WR 43b in HD 97950 of NGC 3603) 132 24,800 11.33 42,000 Spectroscopy SIMBAD [20][21]
HD 269810 (in NGC 2029 of LMC) 130 163,000 12.22 52,500 Spectroscopy SIMBAD [22][23]
Westerhout 49-1 (in Westerhout 49) 130 36,200 15.531 (J band) 44,700 Evolution SIMBAD [5][6]
R136a7 (in Tarantula Nebula of LMC) 127 163,000 13.97 54,000 Evolution SIMBAD [24][8]
WR 42e (in HD 97950 of NGC 3603) 123 25,000 14.53 43,000 Ejection SIMBAD [25][f]
HD 97950 A1a (WR 43a A in HD 97950 of NGC 3603) 120 24,800 11.18 (combined) 42,000 Binary SIMBAD [20][21]
LSS 4067 (in HM 1) 120 11,000 11.44 40,000 Evolution SIMBAD [26][27]
WR 93 (in Pismis 24 of NGC 6357) 120 5,900 10.68 71,000 Evolution SIMBAD [26][15]
Sk -69° 212 (in NGC 2044 of LMC) 119 160,000 12.416 45,400 Evolution SIMBAD [28][19]
Sk -69° 249 A (in NGC 2074 of LMC) 119 160,000 12.02 (combined) 38,900 Evolution SIMBAD [28][29]
ST5-31 (in NGC 2074 of LMC) 119 160,000 12.273 50,700 Evolution SIMBAD [28][30]
R136a5 (in Tarantula Nebula of LMC) 116 157,000 13.71 48,000 Evolution SIMBAD [24][8]
MSP 183 (in Westerlund 2) 115 20,000 13.878 46,300 Spectroscopy SIMBAD [31][32]
WR 24 (in Collinder 228 of Carina Nebula) 114 14,000 6.48 50,100 Evolution SIMBAD [33][34]
HD 97950 C1 (WR 43c A in HD 97950 of NGC 3603) 113 24,800 11.89 (combined) 44,000 Spectroscopy SIMBAD [20][21][e]
Arches-F9 (WR 102ae in Arches Cluster) 111.3 25,000 16.1 (J band) 36,600 Spectroscopy SIMBAD [35][36]
Cygnus OB2 #12 A (in Cygnus OB2) 110 5,200 11.702 (combined) 13,700 Spectroscopy SIMBAD [37][38][e]
HD 93129 Aa (in Trumpler 14 of Carina Nebula) 110 7,500 6.9 (combined) 42,500 Trinary SIMBAD [39][15]
HSH95-36 (in Tarantula Nebula of LMC) 110 163,000 14.41 49,500 Evolution SIMBAD [24][8]
R146 (in Tarantula Nebula of LMC) 109 164,000 13.11 63,000 Spectroscopy SIMBAD [7][8]
R136a4 (in Tarantula Nebula of LMC) 108 157,000 13.41 50,000 Evolution SIMBAD [24][8]
VFTS 621 (in Tarantula Nebula of LMC) 107 164,000 15.39 54,000 Spectroscopy SIMBAD [11][8]
R136a6 (in Tarantula Nebula of LMC) 105 157,000 13.35 52,000 Evolution SIMBAD [24][8]
Westerhout 49-3 (in Westerhout 49) 105 36,200 16.689 (J band) 40,700 Evolution SIMBAD [5][6]
WR 21a A (Runaway star from Westerlund 2) 103.6 26,100 12.661 (combined) 45,000 Binary SIMBAD [40][23]
R99 (in N44 of LMC) 103 164,000 11.52 28,000 Spectroscopy SIMBAD [7][15]
Arches-F6 (WR 102ah in Arches Cluster) 101 25,000 15.75 (J band) 33,900 Spectroscopy SIMBAD [35][36]
Sk -65° 47 (in NGC 1923 of LMC) 101 160,000 12.466 47,800 Evolution SIMBAD [28][19]
Arches-F1 (WR 102ad in Arches Cluster) 100.9 25,000 16.3 (J band) 33,200 Spectroscopy SIMBAD [35][36]
Peony Star (WR 102ka in Peony Nebula near Galactic Center) 100 26,000 12.978 (J band) 25,100 Spectroscopy SIMBAD [41][6]
VFTS 457 (in Tarantula Nebula of LMC) 100 164,000 13.74 39,800 Spectroscopy SIMBAD [11][8]
η Carinae A (in Trumpler 16 of Carina Nebula) 100 7,500 4.3 (combined) 9,400-35,200 Spectroscopy SIMBAD [42][43]
Mercer 30-1 A (WR 46-3 A in Mercer 30 of Dragonfish Nebula) 99 40,000 10.33 (J band) 32,200 Evolution SIMBAD [44][g][e]
Sk -68° 137 (in Tarantula Nebula of LMC) 99 160,000 13.346 50,000 Spectroscopy SIMBAD [18][19]
WR 25 A (in Trumpler 16 of Carina Nebula) 98 6,500 8.8 (combined) 50,100 Evolution SIMBAD [33][15][e]
BI 253 (Runaway star from Tarantula Nebula of LMC) 97.6 164,000 13.76 54,000 Spectroscopy SIMBAD [17][45]
R136a8 (in Tarantula Nebula of LMC) 96 157,000 14.42 49,500 Evolution SIMBAD [24][46]
Westerhout 49-15 (in Westerhout 49) 96 36,200 18.307 (J band) 43,700 Evolution SIMBAD [5][6]
HD 38282 B (in Tarantula Nebula of LMC) 95 163,000 11.11 (combined) 47,000 Binary SIMBAD [47][23]
HM 1-6 (in HM 1) 95 11,000 11.64 44,700 Evolution SIMBAD [26][48]
NGC 3603-42 (in HD 97950 of NGC 3603) 95 25,000 12.86 50,000 Spectroscopy SIMBAD [18][21]
R139 A (in Tarantula Nebula of LMC) 95 163,000 11.94 (combined) 35,000 Binary SIMBAD [7][8]
BAT99-6 (in NGC 1747 of LMC) 94 165,000 11.95 56,000 Spectroscopy SIMBAD [7][19]
Sk -66° 172 (in N64 of LMC) 94 160,000 13.1 46,300 Spectroscopy SIMBAD [18][19][h]
ST2-22 (in NGC 2044 of LMC) 94 160,000 14.3 51,300 Evolution SIMBAD [28][49]
VFTS 259 (in Tarantula Nebula of LMC) 94 164,000 13.65 37,600 Spectroscopy SIMBAD [11][8]
VFTS 562 (in Tarantula Nebula of LMC) 94 164,000 13.66 42,200 Spectroscopy SIMBAD [11][8]
VFTS 512 (in Tarantula Nebula of LMC) 93 164,000 14.28 47,300 Spectroscopy SIMBAD [11][8]
HD 97950 A1b (WR 43a B in HD 97950 of NGC 3603) 92 24,800 11.18 (combined) 40,000 Binary SIMBAD [20][21]
R136b (in Tarantula Nebula of LMC) 92 163,000 13.24 35,500 Evolution SIMBAD [24][8]
VFTS 16 (in Tarantula Nebula of LMC) 91.6 164,000 13.55 50,600 Spectroscopy SIMBAD [17][8]
HD 97950 A3 (in HD 97950 of NGC 3603) 91 24,800 12.95 50,000 Spectroscopy SIMBAD [18][21]
NGC 346-W1 (in NGC 346 of SMC) 91 200,000 12.57 43,400 Evolution SIMBAD [28][50]
R127 (in NGC 2055 of LMC) 90 160,000 10.15 10,000-27,000 Evolution SIMBAD [51][23]
VFTS 333 (in Tarantula Nebula of LMC) 90 164,000 12.49 37,600 Spectroscopy SIMBAD [11][8]
VFTS 267 (in Tarantula Nebula of LMC) 89 164,000 13.49 44,700 Spectroscopy SIMBAD [11][8]
VFTS 64 (in Tarantula Nebula of LMC) 88 164,000 14.621 39,800 Spectroscopy SIMBAD [11][19]
BAT99-80 A (in NGC 2044 of LMC) 87 165,000 13 (combined) 45,000 Spectroscopy SIMBAD [28][49]
R140b (in Tarantula Nebula of LMC) 87 165,000 12.66 47,000 Spectroscopy SIMBAD [7][8]
VFTS 542 (in Tarantula Nebula of LMC) 87 164,000 13.47 44,700 Spectroscopy SIMBAD [11][8]
VFTS 599 (in Tarantula Nebula of LMC) 87 164,000 13.8 44,700 Spectroscopy SIMBAD [11][8]
WR 89 (in HM 1) 87 11,000 11.02 39,800 Evolution SIMBAD [33][23]
Arches-F7 (WR 102aj in Arches Cluster) 86.3 25,000 15.74 (J band) 32,900 Spectroscopy SIMBAD [35][36]
Sk -69° 104 (in NGC 1910 of LMC) 86 160,000 12.1 39,900 Evolution SIMBAD [28][19]
VFTS 1017 (in Tarantula Nebula of LMC) 86 164,000 14.5 50,100 Spectroscopy SIMBAD [11][8]
LH 10-3061 (in NGC 1763 of LMC) 85 160,000 13.491 52,000 Spectroscopy SIMBAD [18][19]
Sk 80 (in NGC 346 of SMC) 85 200,000 12.31 38,900 Evolution SIMBAD [28][52]
VFTS 603 (in Tarantula Nebula of LMC) 85 164,000 13.99 42,200 Spectroscopy SIMBAD [11][8]
Sk -70° 91 (in BSDL 1830 of LMC) 84.09 165,000 12.78 48,900 Evolution SIMBAD [53][19][i]
R147 (in Tarantula Nebula of LMC) 84 164,000 12.993 47,300 Spectroscopy SIMBAD [11][54]
HD 93250 A (in Trumpler 16 of Carina Nebula) 83.3 7,500 7.5 (combined) 46,000 Evolution SIMBAD [55][15][e]
Melnick 33Na A (in Tarantula Nebula of LMC) 83 163,000 13.79 (combined) 50,000 Evolution SIMBAD [56][57]
WR 20a A (in Westerlund 2) 82.7 20,000 13.28 (combined) 43,000 Binary SIMBAD [58]
TIC 276934932 A (in NGC 2048 of LMC) 82 160,000 14.05 (combined) 45,000 Spectroscopy SIMBAD [18][19]
WR 20a B (in Westerlund 2) 81.9 20,000 13.28 (combined) 43,000 Binary SIMBAD [58]
Trumpler 27-27 (in Trumpler 27) 81 3,900 13.31 37,000 Evolution SIMBAD [26][23]
BAT99-96 (in Tarantula Nebula of LMC) 80 165,000 13.76 42,000 Spectroscopy SIMBAD [7][8]
HD 15570 (in IC 1805 of Heart Nebula) 80 7,500 8.11 46,000 Spectroscopy SIMBAD [14][15]
HD 38282 A (in Tarantula Nebula of LMC) 80 163,000 11.11 (combined) 47,000 Binary SIMBAD [47][23]
HSH95-46 (in Tarantula Nebula of LMC) 80 163,000 14.56 47,500 Evolution SIMBAD [24][8]
Arches-F15 (in Arches Cluster) 79.7 25,000 16.12 (J band) 35,600 Spectroscopy SIMBAD [35][36]
BI 237 (in BSDL 2527 of LMC) 79.66 165,000 13.83 51,300 Spectroscopy SIMBAD [53][19][j]
VFTS 94 (in Tarantula Nebula of LMC) 79 164,000 14.161 42,200 Spectroscopy SIMBAD [11][19]
VFTS 151 (in Tarantula Nebula of LMC) 79 164,000 14.13 42,200 Spectroscopy SIMBAD [11][8]
LH 41-32 (in NGC 1910 of LMC) 78 160,000 13.086 48,200 Evolution SIMBAD [28][19]
Pismis 24-17 (in Pismis 24 of NGC 6357) 78 5,900 11.84 42,700 Spectroscopy SIMBAD [59][48]
VFTS 404 (in Tarantula Nebula of LMC) 78 164,000 14.14 44,700 Spectroscopy SIMBAD [11][8]
Westerhout 51-2 (in Westerhout 51) 77 20,000 13.68 (J band) 42,700 Evolution SIMBAD [12]
BAT99-68 (in BSDL 2505 of LMC) 76 165,000 14.13 45,000 Spectroscopy SIMBAD [7][19][k]
HD 93632 (in Collinder 228 of Carina Nebula) 76 10,000 8.23 45,400 Evolution SIMBAD [26][15]
NGC 346-W3 (in NGC 346 of SMC) 76 200,000 12.8 52,500 Evolution SIMBAD [28][50]
VFTS 169 (in Tarantula Nebula of LMC) 76 164,000 14.437 47,300 Spectroscopy SIMBAD [11][19]
VFTS 440 (in Tarantula Nebula of LMC) 76 164,000 12.046 39,800 Spectroscopy SIMBAD [11][19]
AB1 (in DEM S10 of SMC) 75 197,000 15.238 79,000 Spectroscopy SIMBAD [60][50][l]
WR 22 A (in Bochum 10 of Carina Nebula) 75 8,300 6.42 (combined) 44,700 Evolution SIMBAD [33][15][m]
Pismis 24-1NE (in Pismis 24 of NGC 6357) 74 6,500 11 42,500 Binary SIMBAD [59][61]
VFTS 608 (in Tarantula Nebula of LMC) 74 164,000 14.22 42,200 Spectroscopy SIMBAD [11][8]
HSH95-31 (in Tarantula Nebula of LMC) 73 163,000 14.12 47,500 Evolution SIMBAD [24][8]
Mercer 30-3 (in Mercer 30 of Dragonfish Nebula) 73 40,000 12.62 (J band) 39,300 Evolution SIMBAD [44][g]
Mercer 30-11 (in Mercer 30 of Dragonfish Nebula) 73 40,000 12.33 (J band) 36,800 Evolution SIMBAD [44][g]
VFTS 566 (in Tarantula Nebula of LMC) 73 164,000 14.05 44,700 Spectroscopy SIMBAD [11][8]
LH 64-16 (in NGC 2001 of LMC) 72 160,000 13.666 50,900 Evolution SIMBAD [28][30]
NGC 2044-W35 (in NGC 2044 of LMC) 72 160,000 14.1 48,200 Evolution SIMBAD [28][19]
VFTS 216 (in Tarantula Nebula of LMC) 72 164,000 14.389 44,700 Spectroscopy SIMBAD [11][19]
ST2-1 (in NGC 2044 of LMC) 71 160,000 14.3 44,100 Evolution SIMBAD [28][49]
VFTS 3 (in Tarantula Nebula of LMC) 71 164,000 11.56 21,000 Spectroscopy SIMBAD [62][8]
Arches-F12 (WR 102af in Arches Cluster) 70 25,000 16.4 (J band) 36,900 Spectroscopy SIMBAD [35][36]
HD 15629 (in IC 1805 of Heart Nebula) 70 7,500 8.42 45,900 Spectroscopy SIMBAD [14][15]
HD 37974 (in N135 of LMC) 70 163,000 10.99 22,500 Spectroscopy SIMBAD [63][23][n]
HD 93129 Ab (in Trumpler 14 of Carina Nebula) 70 7,500 7.31 (combined) 44,000 Trinary SIMBAD [39][64]
M33 X-7 B (in Triangulum Galaxy) 70 2,700,000 18.7 35,000 Binary SIMBAD [65][66]
Sk -69° 194 A (in NGC 2033 of LMC) 70 160,000 12.131 (combined) 45,000 Evolution SIMBAD [28][54][e]
VFTS 125 (in Tarantula Nebula of LMC) 69.6 164,000 16.6 55,200 Spectroscopy SIMBAD [17][49]
HD 46150 (in NGC 2244 of Rosette Nebula) 69 5,200 6.73 44,000 Spectroscopy SIMBAD [18][15]
HD 229059 (in Berkeley 87) 69 3,000 8.7 26,300 Evolution SIMBAD [26][15]
ST2-3 (in NGC 2044 of LMC) 69 160,000 14.264 44,900 Evolution SIMBAD [28][19]
ST2-32 (in NGC 2044 of LMC) 69 160,000 13.903 45,400 Evolution SIMBAD [28][19]
W28-23 (in NGC 2033 of LMC) 69 160,000 13.702 51,300 Evolution SIMBAD [28][30]
HD 93403 A (in Trumpler 16 of Carina Nebula) 68.5 10,400 8.27 (combined) 39,300 Binary SIMBAD [67][23]
HD 93130 (in Collinder 228 of Carina Nebula) 68 10,000 8.04 39,900 Evolution SIMBAD [26][15]
HM 1-8 (in HM 1) 68 11,000 12.52 46,100 Evolution SIMBAD [26][48]
HSH95-47 (in Tarantula Nebula of LMC) 68 163,000 14.72 43,500 Evolution SIMBAD [24][8]
HSH95-48 (in Tarantula Nebula of LMC) 68 163,000 14.75 46,500 Evolution SIMBAD [24][46]
Westerhout 51-61 (in Westerhout 51) 68 20,000 18.16 (J band) 38,000 Evolution SIMBAD [12][6]
BAT99-93 (in Tarantula Nebula of LMC) 67 165,000 13.446 45,000 Spectroscopy SIMBAD [7][19]
Sk -69° 200 (in NGC 2033 of LMC) 67 160,000 11.18 26,300 Evolution SIMBAD [28][19]
Arches-F18 (in Arches Cluster) 66.9 25,000 16.7 (J band) 36,900 Spectroscopy SIMBAD [35][36]
Arches-F4 (WR 102al in Arches Cluster) 66.4 25,000 15.63 (J band) 36,800 Spectroscopy SIMBAD [35][36]
BAT99-59 A (in NGC 2020 of LMC) 66 165,000 13.186 (combined) 71,000 Spectroscopy SIMBAD [7][19][e]
BAT99-104 (in Tarantula Nebula of LMC) 66 165,000 12.5 63,000 Spectroscopy SIMBAD [7][19]
HD 5980 B (in NGC 346 of SMC) 66 200,000 11.31 (combined) 45,000 Trinary SIMBAD [68][64]
HD 190429 A (near Barnard 146) 66 7,800 6.63 (combined) 46,000 Binary SIMBAD [69][15]
LH 31-1003 (in NGC 1858 of LMC) 66 160,000 13.186 41,900 Evolution SIMBAD [28][19]
LH 114-7 (in N70 of LMC) 66 160,000 13.66 50,000 Spectroscopy SIMBAD [18][19][o]
Pismis 24-1SW (in Pismis 24 of NGC 6357) 66 6,500 11.1 40,000 Binary SIMBAD [59][61]
BAT99-126 (in NGC 2081 of LMC) 65 165,000 13.166 71,000 Spectroscopy SIMBAD [7][19]
HSH95-40 (in Tarantula Nebula of LMC) 65 163,000 14.56 47,500 Evolution SIMBAD [24][8]
HSH95-58 (in Tarantula Nebula of LMC) 65 163,000 14.8 47,500 Evolution SIMBAD [24][8]
HSH95-89 (in Tarantula Nebula of LMC) 65 163,000 14.76 44,000 Spectroscopy SIMBAD [46]
VFTS 63 (in Tarantula Nebula of LMC) 65 164,000 14.4 42,200 Spectroscopy SIMBAD [11][49]
VFTS 145 (in Tarantula Nebula of LMC) 65 164,000 14.3 39,800 Spectroscopy SIMBAD [11][8]
VFTS 518 (in Tarantula Nebula of LMC) 65 164,000 15.11 44,700 Spectroscopy SIMBAD [11][8]
Westerhout 49-8 (in Westerhout 49) 65 36,200 15.617 (J band) 40,700 Evolution SIMBAD [5][6]
BD+43° 3654 (Runaway star from Cygnus OB2) 64.6 5,400 10.06 40,400 Evolution SIMBAD [70][64]
BAT99-129 A (in DEM L294 of LMC) 64 165,000 14.701 (combined) 79,000 Spectroscopy SIMBAD [7][19][p][e]
HSH95-50 (in Tarantula Nebula of LMC) 64 163,000 14.65 47,000 Evolution SIMBAD [24][8]
Sk -69° 25 (in NGC 1748 of LMC) 64 160,000 11.886 43,600 Evolution SIMBAD [28][19]
Trumpler 27-23 (in Trumpler 27) 64 3,900 10.09 27,500 Evolution SIMBAD [26][23]
Westerhout 49-5 (in Westerhout 49) 64 36,200 15.623 (J band) 42,700 Evolution SIMBAD [5][6]
HD 46223 (in NGC 2244 of Rosette Nebula) 63 5,200 7.28 46,000 Spectroscopy SIMBAD [18][15]
HD 64568 (in NGC 2467 of Puppis OB2) 63 16,000 9.39 54,000 Spectroscopy SIMBAD [18][23]
HD 303308 (in Trumpler 16 of Carina Nebula) 63 9,200 8.17 51,300 Evolution SIMBAD [26][23]
HR 6187 A (in NGC 6193 of Ara OB1) 63 4,300 5.54 (combined) 46,500 Septenary SIMBAD [71][15]
LH 10-3058 (in NGC 1763 of LMC) 63 160,000 14.089 54,000 Spectroscopy SIMBAD [18][19]
ST5-71 (in NGC 2074 of LMC) 63 160,000 13.266 45,400 Evolution SIMBAD [28][19]
AB9 (in DEM S80 of SMC) 62 197,000 15.431 100,000 Spectroscopy SIMBAD [60][50][q]
Brey 32 B (in NGC 1966 of LMC) 62 165,000 12.32 (combined) 43,600 Evolution SIMBAD [28][23]
HD 93160 (in Trumpler 14 of Carina Nebula) 62 8,000 7.6 42,700 Evolution SIMBAD [26][15]
HSH95-35 (in Tarantula Nebula of LMC) 62 163,000 14.43 47,500 Evolution SIMBAD [24][8]
LH 41-1017 (in NGC 1910 of LMC) 62 160,000 12.266 42,700 Evolution SIMBAD [28][19]
Mercer 30-6a A (WR 46-4 A in Mercer 30 of Dragonfish Nebula) 62 40,000 10.39 (J band) 29,900 Evolution SIMBAD [44][g][e]
ST4-18 (in NGC 2081 of LMC) 62 160,000 13.639 44,800 Evolution SIMBAD [28][19]
VFTS 664 (in Tarantula Nebula of LMC) 62 164,000 13.937 39,900 Spectroscopy SIMBAD [11][19]
HD 229196 (in Cygnus OB9) 61.6 5,000 8.59 40,900 Evolution SIMBAD [70][48]
AB8 B (in NGC 602 of SMC) 61 197,000 12.83 (combined) 45,000 Binary SIMBAD [68][72]
BAT99-79 A (in NGC 2044 of LMC) 61 165,000 13.486 (combined) 42,000 Spectroscopy SIMBAD [7][19][e]
HD 5980 A (in NGC 346 of SMC) 61 200,000 11.31 (combined) 21,000-53,000 Trinary SIMBAD [68][64]
LH 41-18 (in NGC 1910 of LMC) 61 160,000 12.586 38,500 Evolution SIMBAD [28][19]
Mercer 30-9 A (in Mercer 30 of Dragonfish Nebula) 61 40,000 12.25 (J band) 34,500 Evolution SIMBAD [44][g][e]
ST5-25 (in NGC 2074 of LMC) 61 160,000 13.551 48,600 Evolution SIMBAD [28][30]
VFTS 422 (in Tarantula Nebula of LMC) 61 164,000 15.14 39,800 Spectroscopy SIMBAD [11][8]
WR 102hb (in Quintuplet cluster) 61 26,000 13.9 (J band) 25,100 Evolution SIMBAD [73][74]
Sk -67° 166 (in GKK-A144 of LMC) 60.68 160,000 12.22 41,800 Spectroscopy SIMBAD [53][19][r]
Sk -67° 167 (in GKK-A144 of LMC) 60.68 160,000 12.586 41,800 Spectroscopy SIMBAD [53][19][r]
Sk -71° 46 (in BSDL 2242 of LMC) 60.68 160,000 13.241 41,800 Spectroscopy SIMBAD [53][19][s]
Brey 10 (in NGC 1770 of LMC) 60 165,000 12.69 117,000 Evolution SIMBAD [28][23]
Brey 94 A (in NGC 2081 of LMC) 60 165,000 12.996 (combined) 83,000 Evolution SIMBAD [28][19][e]
Brey 95a A (in NGC 2081 of LMC) 60 165,000 12.2 (combined) 83,000 Evolution SIMBAD [28][75][e]
HSH95-55 (in Tarantula Nebula of LMC) 60 163,000 14.74 47,500 Evolution SIMBAD [24][8]
Mercer 30-7 A (WR 46-5 A in Mercer 30 of Dragonfish Nebula) 60 40,000 11.516 (J band) 41,400 Evolution SIMBAD [44][g][e]
R134 (in Tarantula Nebula of LMC) 60 164,000 12.75 39,800 Spectroscopy SIMBAD [11][8]
R142 (in Tarantula Nebula of LMC) 60 164,000 11.82 18,000 Spectroscopy SIMBAD [62][8]
R143 (in Tarantula Nebula of LMC) 60 160,000 12.014 18,000-36,000 Evolution SIMBAD [51][19]
Sk -69° 142a (in NGC 1983 of LMC) 60 160,000 11.093 34,000 Evolution SIMBAD [51][54]
Sk -69° 259 (in NGC 2081 of LMC) 60 160,000 11.93 23,000 Evolution SIMBAD [28][23]
Var 83 (in Triangulum Galaxy) 60 3,000,000 16.027 18,000-37,000 Evolution SIMBAD [76][77]
VFTS 430 (in Tarantula Nebula of LMC) 60 164,000 15.11 24,500 Spectroscopy SIMBAD [62][8]

A few notable stars of mass less than 60 M☉ are included for the purpose of comparison.

Star name Mass
(M☉, Sun = 1) 		Approx. distance
from earth (ly) 		Apparent
visible magnitude 		Effective
temperature (K) 		Estimation
method 		Link Reference
ζ Puppis (Naos in Vela R2 of Vela Molecular Ridge) 56.1 1,080 2.25 40,000 Spectroscopy SIMBAD [69][15][t]
λ Cephei (Runaway star from Cepheus OB3) 51.4 3,100 5.05 36,000 Spectroscopy SIMBAD [69][15]
τ Canis Majoris Aa (in NGC 2362) 50 5,120 4.89 32,000 Evolution SIMBAD [78][15]
θ Muscae Ab (in Centaurus OB1) 44 7,400 5.53 (combined) 33,000 Evolution SIMBAD [79][15]
ε Orionis (Alnilam in Orion OB1 of Orion complex) 40 2,000 1.69 27,500 Evolution SIMBAD [80][15]
θ2 Orionis A (in Orion OB1 of Orion complex) 39 1,500 5.02 34,900 Evolution SIMBAD [81][82]
α Camelopardalis (Runaway star from NGC 1502) 37.6 6,000 4.29 29,000 Evolution SIMBAD [83][15]
P Cygni (in IC 4996 of Cygnus OB1) 37 5,100 4.82 18,700 Spectroscopy SIMBAD [84][15][u]
ζ1 Scorpii (in NGC 6231 of Scorpius OB1) 36 8,210 4.705 17,200 Spectroscopy SIMBAD [37][85]
ζ Orionis Aa (Alnitak in Orion OB1 of Orion complex) 33 1,260 2.08 29,500 Evolution SIMBAD [86]
θ1 Orionis C1 (in Trapezium Cluster of Orion complex) 33 1,340 5.13 (combined) 39,000 Evolution SIMBAD [87][15]
κ Cassiopeiae (in Cassiopeia OB14) 33 4,000 4.16 23,500 Evolution SIMBAD [88][15]
μ Normae (in NGC 6169) 33 3,260 4.91 28,000 Spectroscopy SIMBAD [89][15]
η Carinae B (in Trumpler 16 of Carina Nebula) 30 7,500 4.3 (combined) 37,200 Binary SIMBAD [90][43]
γ2 Velorum B (in Vela OB2) 28.5 1,230 1.83 (combined) 35,000 Evolution SIMBAD [91][15]
λ Orionis A (Meissa in Collinder 69 of Orion complex) 27.9 1,100 3.54 37,700 Spectroscopy SIMBAD [89][92]
ξ Persei (Menkib in California Nebula of Perseus OB2) 26.1 1,200 4.04 35,000 Evolution SIMBAD [83][15]
WR 79a (in NGC 6231 of Scorpius OB1) 24.4 5,600 5.77 35,000 Spectroscopy SIMBAD [89][15]
δ Orionis Aa1 (Mintaka in Orion OB1 of Orion complex) 24 1,200 2.5 (combined) 29,500 Evolution SIMBAD [93][94]
ι Orionis Aa1 (Hatysa in NGC 1980 of Orion complex) 23.1 1,340 2.77 (combined) 32,500 Evolution SIMBAD [95][96]
κ Crucis (in Jewel Box Cluster of Centaurus OB1) 23 7,500 5.98 16,300 Evolution SIMBAD [97][64]
WR 78 (in NGC 6231 of Scorpius OB1) 22 4,100 6.48 50,100 Spectroscopy SIMBAD [33][34]
ο2 Canis Majoris (in Collinder 121) 21.4 2,800 3.043 15,500 Evolution SIMBAD [89][15]
β Orionis A (Rigel in Orion OB1 of Orion complex) 21 860 0.13 12,100 Evolution SIMBAD [98][15]
η Canis Majoris (Aludra in Collinder 121) 21 2,000 2.45 15,000 Evolution SIMBAD [88][15]
ζ Ophiuchi (in Upper Scorpius subgroup of Scorpius OB2) 20.2 370 2.569 34,000 Evolution SIMBAD [83][15]
υ Orionis (in Orion OB1 of Orion complex) 20 2,900 4.618 33,400 Evolution SIMBAD [99][100]
σ Orionis Aa (in Orion OB1 of Orion complex) 18 1,260 4.07 (combined) 35,000 Spectroscopy SIMBAD [101][102]
μ Columbae (Runaway star from Trapezium Cluster) 16 1,300 5.18 33,000 Spectroscopy SIMBAD [103][15]
κ Orionis (Saiph in Orion OB1 of Orion complex) 15.5 650 2.09 26,500 Evolution SIMBAD [104][15]
σ Cygni (in Cygnus OB4) 15 3,260 4.233 10,800 Evolution SIMBAD [105][106]
θ Carinae A (in IC 2602 of Scorpius OB2) 14.9 460 2.76 (combined) 31,000 Evolution SIMBAD [89][107]
θ2 Orionis B (in Orion OB1 of Orion complex) 14.8 1,500 6.38 29,300 Spectroscopy SIMBAD [108]
ζ Persei (in Perseus OB2) 14.5 750 2.86 20,800 Evolution SIMBAD [104][15]
σ Orionis B (in Orion OB1 of Orion complex) 14 1,260 4.07 (combined) 31,000 Spectroscopy SIMBAD [101][102]
β Canis Majoris (Mirzam in Local Bubble of Scorpius OB2) 13.5 490 1.985 23,200 Evolution SIMBAD [109][110]
ε Persei A (in α Persei Cluster) 13.5 640 2.88 (combined) 26,500 Evolution SIMBAD [111][112]
ι Orionis Aa2 (in NGC 1980 of Orion complex) 13.1 1,340 2.77 (combined) 27,000 Evolution SIMBAD [95][96]
δ Scorpii A (Dschubba in Upper Scorpius subgroup of Scorpius OB2) 13 440 2.307 (combined) 27,400 Evolution SIMBAD [113][114]
σ Orionis Ab (in Orion OB1 of Orion complex) 13 1,260 4.07 (combined) 29,000 Spectroscopy SIMBAD [101][102]
θ Muscae Aa (WR 48 in Centaurus OB1) 11.5 7,400 5.53 (combined) 83,000 Spectroscopy SIMBAD [115][15]
γ2 Velorum A (WR 11 in Vela OB2) 9 1,230 1.83 (combined) 57,000 Spectroscopy SIMBAD [91][15]
ρ Ophiuchi A (in ρ Ophiuchi cloud complex of Scorpius OB2) 8.7 360 4.63 (combined) 22,000 Evolution SIMBAD [89][15]
γ Orionis (Bellatrix in Bellatrix Cluster of Orion complex) 7.7 250 1.64 21,800 Evolution SIMBAD [116][15]
α Scorpii B (in Loop I Bubble of Scorpius OB2) 7.2 550 5.5 18,500 Evolution SIMBAD [117][92]
λ Tauri A (in Pisces-Eridanus stellar stream) 7.18 480 3.47 (combined) 18,700 Evolution SIMBAD [118][119]
δ Persei (in α Persei Cluster) 7 520 3.01 14,900 Evolution SIMBAD [89][107]
ψ Persei (in α Persei Cluster) 6.2 580 4.31 16,000 Evolution SIMBAD [89][15]
α Pavonis Aa (Peacock in Tucana-Horologium association) 5.91 180 1.94 17,700 Evolution SIMBAD [120][96]
η Tauri A (Alcyone in Pleiades) 5.9 440 2.87 (combined) 12,300 Evolution SIMBAD [121][15]
γ Canis Majoris (Muliphein in Collinder 121) 5.6 440 4.1 13,600 Evolution SIMBAD [89][122]
ο Velorum (in IC 2391 of Scorpius OB2) 5.5 490 3.6 16,200 Evolution SIMBAD [123][107]
ο Aquarii (in Pisces-Eridanus stellar stream) 4.2 440 4.71 13,500 Evolution SIMBAD [124][125]
ν Fornacis (in Pisces-Eridanus stellar stream) 3.65 370 4.69 13,400 Evolution SIMBAD [126][15]
φ Eridani (in Tucana-Horologium association) 3.55 150 3.55 13,700 Evolution SIMBAD [120][127]
η Chamaeleontis (in η Chamaeleontis moving group of Scorpius OB2) 3.2 310 5.453 12,500 Evolution SIMBAD [128][64]
ε Chamaeleontis (in ε Chamaeleontis moving group of Scorpius OB2) 2.87 360 4.91 10,900 Evolution SIMBAD [129][107]
τ1 Aquarii (in Pisces-Eridanus stellar stream) 2.68 320 5.66 10,600 Evolution SIMBAD [130][131]
ε Hydri (in Tucana-Horologium association) 2.64 150 4.12 11,000 Evolution SIMBAD [130][132]
β1 Tucanae (in Tucana-Horologium association) 2.5 140 4.37 10,600 Evolution SIMBAD [89][92]
Sun (in Solar System) 1 0.0000158 −26.744 5,772 Standard IAU [133][134][135]
  1. ^ For some methods, different determinations of chemical composition lead to different estimates of mass.
  2. ^ For a binary star, it is possible to measure the individual masses of the two stars by studying their orbital motions, using Kepler's laws of planetary motion.
  3. ^ The superwinds from massive stars are similar to the superwinds generated by asymptotic giant branch (AGB) stars – red giants – that form planetary nebulae. These stars' later remnants become the (technically non-stellar) white dwarf cores of planetary nebulae.
  4. ^ For examples of stellar debris see hypernovae and supernova remnant.
  5. ^ a b c d e f g h i j k l m n o This is a binary system but the secondary is much less massive than the primary.
  6. ^ This unusual measurement was made by assuming the star was ejected from a three-body encounter in NGC 3603. This assumption also means that the current star is the result of a merger between two original close binary components. The mass is consistent with evolutionary mass for a star with the observed parameters.
  7. ^ a b c d e f Mercer 30 is an open cluster in Dragonfish Nebula.
  8. ^ N64 is an emission nebula in Large Magellanic Cloud.
  9. ^ BSDL 1830 is a star cluster in Large Magellanic Cloud.
  10. ^ BSDL 2527 is a star cluster in Large Magellanic Cloud.
  11. ^ BSDL 2505 is a star cluster in Large Magellanic Cloud.
  12. ^ DEM S10 is a H II region in Small Magellanic Cloud.
  13. ^ Bochum 10 is an open cluster in Carina Nebula.
  14. ^ N135 is an emission nebula in Large Magellanic Cloud.
  15. ^ N70 is an emission nebula in Large Magellanic Cloud.
  16. ^ DEM L294 is a H II region in Large Magellanic Cloud.
  17. ^ DEM S80 is a H II region in Small Magellanic Cloud.
  18. ^ a b GKK-A144 is a stellar association in Large Magellanic Cloud.
  19. ^ BSDL 2242 is a star cluster in Large Magellanic Cloud.
  20. ^ Vela R2 is a OB association in Vela Molecular Ridge.
  21. ^ IC 4996 is an open cluster in Cygnus OB1.

Black holes

Main articles: Black hole, List of black holes, and List of most massive black holes

Black holes are the end point evolution of massive stars. Technically they are not stars, as they no longer generate heat and light via nuclear fusion in their cores. Some black holes may have cosmological origins, and would then never have been stars. This is thought to be especially likely in the cases of the most massive black holes.

See also

References

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External links

  • "Statistics in Arches cluster". HubbleSite. May 2005.
  • "Most Massive Star Discovered". Space.com. 7 June 2007.
  • "Arches cluster". ScienceDaily. March 2005.
  • . 3towers. Archived from the original on 2007-10-28.
  • "Hubble Unveils Monster Stars". NASA. March 2016.
February 20, 2023
list, most, massive, stars, this, article, about, mass, radius, list, largest, stars, this, list, most, massive, stars, that, have, been, discovered, solar, masses, contents, uncertainties, caveats, complications, with, distance, obscuring, clouds, rare, relia. This article is about mass For radius see List of largest stars This is a list of the most massive stars that have been discovered in solar masses M Contents 1 Uncertainties and caveats 1 1 Complications with distance and obscuring clouds 1 2 Rare reliable estimates 1 3 Relevance of stellar evolution 1 4 Mass limits 1 4 1 Accretion limits 1 4 2 Eddington mass limit 2 List of the most massive stars 3 Black holes 4 See also 5 References 6 External linksUncertainties and caveats EditMost of the masses listed below are contested and being the subject of current research remain under review and subject to constant revision of their masses and other characteristics Indeed many of the masses listed in the table below are inferred from theory using difficult measurements of the stars temperatures and absolute brightnesses All the masses listed below are uncertain Both the theory and the measurements are pushing the limits of current knowledge and technology Both theories and measurements could be incorrect For example VV Cephei could be between 25 40 M or 100 M depending on which property of the star is examined Artist s impression of disc of obscuring material around a massive star Complications with distance and obscuring clouds Edit Since massive stars are rare astronomers must look very far from Earth to find them All the listed stars are many thousands of light years away which makes measurements difficult In addition to being far away many stars of such extreme mass are surrounded by clouds of outflowing gas created by extremely powerful stellar winds the surrounding gas interferes with the already difficult to obtain measurements of stellar temperatures and brightnesses which greatly complicates the issue of estimating internal chemical compositions and structures a This obstruction leads to difficulties in calculating parameters Eta Carinae is the bright spot hidden in the double lobed dust cloud It is the most massive star that has a Bayer designation It was only discovered to be at least two stars in the past few decades Both the obscuring clouds and the great distances make it difficult to judge whether the star is just a single supermassive object or instead a multiple star system A number of the stars listed below may actually be two or more companions orbiting too closely to distinguish by our telescopes each star being massive in itself but not necessarily supermassive to either be on this list or near the top of it Other combinations are possible for example a supermassive star with one or more smaller companions or more than one giant star but without being able to see inside the surrounding cloud it is difficult to know the truth of the matter More globally statistics on stellar populations seem to indicate that the upper mass limit is in the 100 200 solar mass range 1 so all mass estimates exceeding this range are suspect Rare reliable estimates Edit Eclipsing binary stars are the only stars whose masses are estimated with some confidence However note that almost all of the masses listed in the table below were inferred by indirect methods only a few of the masses in the table were determined using eclipsing systems WR 25 is a binary star whose orbit around its obscured companion provided a constraint on its mass Amongst the most reliable listed masses are those for the eclipsing binaries NGC 3603 A1 WR 21a and WR 20a Masses for all three were obtained from orbital measurements b This involves measuring their radial velocities and also their light curves The radial velocities only yield minimum values for the masses depending on inclination but light curves of eclipsing binaries provide the missing information inclination of the orbit to our line of sight Relevance of stellar evolution Edit Some stars may once have been more massive than they are today It is likely that many large stars have suffered significant mass loss perhaps as much as several tens of solar masses This mass may have been expelled by superwinds high velocity winds that are driven by the hot photosphere into interstellar space The process forms an enlarged extended envelope around the star that interacts with the nearby interstellar medium and infusing the region with elements heavier than hydrogen or helium c There are also or rather were stars that might have appeared on the list but no longer exist as stars or are supernova impostors today we see only their debris d The masses of the precursor stars that fueled these destructive events can be estimated from the type of explosion and the energy released but those masses are not listed here see Black holes below Mass limits Edit There are two related theoretical limits on how massive a star can possibly be the accretion limit and the Eddington mass limit The accretion limit is related to star formation After about 120 M have accreted in a protostar the combined mass should have become hot enough for its heat to drive away any further incoming matter In effect the protostar reaches a point where it evaporates away material as fast as it collects new material The Eddington limit is based on light pressure from the core of an already formed star As mass increases past 150 M the intensity of light radiated from a Population I star s core will become sufficient for the light pressure pushing outward to exceed the gravitational force pulling inward and the surface material of the star will be free to float away into space Accretion limits Edit Astronomers have long hypothesized that as a protostar grows to a size beyond 120 M something drastic must happen 2 Although the limit can be stretched for very early Population III stars and although the exact value is uncertain if any stars still exist above 150 200 M they would challenge current theories of stellar evolution Studying the Arches Cluster which is currently the densest known cluster of stars in our galaxy astronomers have confirmed that no stars in that cluster exceed about 150 M The R136 cluster is an unusually dense collection of young hot blue stars Rare ultramassive stars that exceed this limit for example in the R136 star cluster might be explained by the following proposal Some of the pairs of massive stars in close orbit in young unstable multiple star systems must occasionally collide and merge where certain unusual circumstances hold that make a collision possible 3 Eddington mass limit Edit Main article Eddington luminosity A limit on stellar mass arises because of light pressure For a sufficiently massive star the outward pressure of radiant energy generated by nuclear fusion in the star s core exceeds the inward pull of its own gravity The lowest mass for which this effect is active is the Eddington limit Stars of greater mass have a higher rate of core energy generation and heavier stars luminosities increase far out of proportion to the increase in their masses The Eddington limit is the point beyond which a star ought to push itself apart or at least shed enough mass to reduce its internal energy generation to a lower maintainable rate The actual limit point mass depends on how opaque the gas in the star is and metal rich Population I stars have lower mass limits than metal poor Population II stars Before their demise the hypothetical metal free Population III stars would have had the highest allowed mass somewhere around 300 M In theory a more massive star could not hold itself together because of the mass loss resulting from the outflow of stellar material In practice the theoretical Eddington Limit must be modified for high luminosity stars and the empirical Humphreys Davidson limit is used instead 4 List of the most massive stars EditLegend Wolf Rayet starLuminous blue variableO type starB type starThe following two lists show a few of the known stars including the stars in open cluster OB association and H II region Despite their high luminosity many of them are nevertheless too distant to be observed with the naked eye Stars that are at least sometimes visible to the unaided eye have their apparent magnitude 6 5 or brighter highlighted in blue The first list gives stars that are estimated to be 60 M or larger the majority of which are shown The second list includes some notable stars which are below 60 M for the purpose of comparison The method used to determine each star s mass is included to give an idea of the data s uncertainty note that the mass of binary stars can be determined far more accurately The masses listed below are the stars current evolved mass not their initial formation mass This list is incomplete you can help by adding missing items January 2016 Stars with 60 M or greater Star name Mass M Sun 1 Approx distancefrom Earth ly Apparentvisible magnitude Effectivetemperature K Estimationmethod Link ReferenceWesterhout 49 2 in Westerhout 49 250 36 200 18 246 J band 35 500 Spectroscopy SIMBAD 5 6 BAT99 98 in Tarantula Nebula of LMC 226 165 000 13 37 45 000 Spectroscopy SIMBAD 7 8 R136a1 in Tarantula Nebula of LMC 196 163 000 12 23 46 000 Evolution SIMBAD 9 10 Melnick 42 in Tarantula Nebula of LMC 189 163 000 12 78 47 300 Spectroscopy SIMBAD 11 8 VFTS 1022 in Tarantula Nebula of LMC 178 164 000 13 47 42 200 Spectroscopy SIMBAD 11 8 Westerhout 51 57 in Westerhout 51 160 20 000 16 66 J band 42 700 Evolution 12 R136a3 in Tarantula Nebula of LMC 155 163 000 12 97 50 000 Evolution SIMBAD 9 10 VFTS 682 in Tarantula Nebula of LMC 153 164 000 16 08 52 200 Spectroscopy SIMBAD 13 8 HD 15558 A in IC 1805 of Heart Nebula 152 24 400 7 87 combined 39 500 Binary SIMBAD 14 15 R136a2 in Tarantula Nebula of LMC 151 163 000 12 34 50 000 Evolution SIMBAD 9 10 Westerhout 51 3 in Westerhout 51 148 20 000 17 79 J band 39 800 Evolution SIMBAD 12 Melnick 34 A in Tarantula Nebula of LMC 147 163 000 13 09 combined 53 000 Binary SIMBAD 16 8 VFTS 482 in Tarantula Nebula of LMC 145 164 000 12 95 42 200 Spectroscopy SIMBAD 11 8 R136c in Tarantula Nebula of LMC 142 163 000 13 43 51 000 Evolution SIMBAD 17 8 VFTS 1021 in Tarantula Nebula of LMC 141 164 000 13 35 39 800 Spectroscopy SIMBAD 11 8 LH 10 3209 A in NGC 1763 of LMC 140 160 000 11 859 combined 42 500 Spectroscopy SIMBAD 18 19 e VFTS 506 in Tarantula Nebula of LMC 138 164 000 13 31 47 300 Spectroscopy SIMBAD 13 8 Melnick 34 B in Tarantula Nebula of LMC 136 163 000 13 09 combined 53 000 Binary SIMBAD 16 8 Westerhout 51d in Westerhout 51 135 20 000 15 11 J band 42 700 Evolution 12 VFTS 545 in Tarantula Nebula of LMC 133 164 000 13 32 47 300 Spectroscopy SIMBAD 11 8 HD 97950 B WR 43b in HD 97950 of NGC 3603 132 24 800 11 33 42 000 Spectroscopy SIMBAD 20 21 HD 269810 in NGC 2029 of LMC 130 163 000 12 22 52 500 Spectroscopy SIMBAD 22 23 Westerhout 49 1 in Westerhout 49 130 36 200 15 531 J band 44 700 Evolution SIMBAD 5 6 R136a7 in Tarantula Nebula of LMC 127 163 000 13 97 54 000 Evolution SIMBAD 24 8 WR 42e in HD 97950 of NGC 3603 123 25 000 14 53 43 000 Ejection SIMBAD 25 f HD 97950 A1a WR 43a A in HD 97950 of NGC 3603 120 24 800 11 18 combined 42 000 Binary SIMBAD 20 21 LSS 4067 in HM 1 120 11 000 11 44 40 000 Evolution SIMBAD 26 27 WR 93 in Pismis 24 of NGC 6357 120 5 900 10 68 71 000 Evolution SIMBAD 26 15 Sk 69 212 in NGC 2044 of LMC 119 160 000 12 416 45 400 Evolution SIMBAD 28 19 Sk 69 249 A in NGC 2074 of LMC 119 160 000 12 02 combined 38 900 Evolution SIMBAD 28 29 ST5 31 in NGC 2074 of LMC 119 160 000 12 273 50 700 Evolution SIMBAD 28 30 R136a5 in Tarantula Nebula of LMC 116 157 000 13 71 48 000 Evolution SIMBAD 24 8 MSP 183 in Westerlund 2 115 20 000 13 878 46 300 Spectroscopy SIMBAD 31 32 WR 24 in Collinder 228 of Carina Nebula 114 14 000 6 48 50 100 Evolution SIMBAD 33 34 HD 97950 C1 WR 43c A in HD 97950 of NGC 3603 113 24 800 11 89 combined 44 000 Spectroscopy SIMBAD 20 21 e Arches F9 WR 102ae in Arches Cluster 111 3 25 000 16 1 J band 36 600 Spectroscopy SIMBAD 35 36 Cygnus OB2 12 A in Cygnus OB2 110 5 200 11 702 combined 13 700 Spectroscopy SIMBAD 37 38 e HD 93129 Aa in Trumpler 14 of Carina Nebula 110 7 500 6 9 combined 42 500 Trinary SIMBAD 39 15 HSH95 36 in Tarantula Nebula of LMC 110 163 000 14 41 49 500 Evolution SIMBAD 24 8 R146 in Tarantula Nebula of LMC 109 164 000 13 11 63 000 Spectroscopy SIMBAD 7 8 R136a4 in Tarantula Nebula of LMC 108 157 000 13 41 50 000 Evolution SIMBAD 24 8 VFTS 621 in Tarantula Nebula of LMC 107 164 000 15 39 54 000 Spectroscopy SIMBAD 11 8 R136a6 in Tarantula Nebula of LMC 105 157 000 13 35 52 000 Evolution SIMBAD 24 8 Westerhout 49 3 in Westerhout 49 105 36 200 16 689 J band 40 700 Evolution SIMBAD 5 6 WR 21a A Runaway star from Westerlund 2 103 6 26 100 12 661 combined 45 000 Binary SIMBAD 40 23 R99 in N44 of LMC 103 164 000 11 52 28 000 Spectroscopy SIMBAD 7 15 Arches F6 WR 102ah in Arches Cluster 101 25 000 15 75 J band 33 900 Spectroscopy SIMBAD 35 36 Sk 65 47 in NGC 1923 of LMC 101 160 000 12 466 47 800 Evolution SIMBAD 28 19 Arches F1 WR 102ad in Arches Cluster 100 9 25 000 16 3 J band 33 200 Spectroscopy SIMBAD 35 36 Peony Star WR 102ka in Peony Nebula near Galactic Center 100 26 000 12 978 J band 25 100 Spectroscopy SIMBAD 41 6 VFTS 457 in Tarantula Nebula of LMC 100 164 000 13 74 39 800 Spectroscopy SIMBAD 11 8 h Carinae A in Trumpler 16 of Carina Nebula 100 7 500 4 3 combined 9 400 35 200 Spectroscopy SIMBAD 42 43 Mercer 30 1 A WR 46 3 A in Mercer 30 of Dragonfish Nebula 99 40 000 10 33 J band 32 200 Evolution SIMBAD 44 g e Sk 68 137 in Tarantula Nebula of LMC 99 160 000 13 346 50 000 Spectroscopy SIMBAD 18 19 WR 25 A in Trumpler 16 of Carina Nebula 98 6 500 8 8 combined 50 100 Evolution SIMBAD 33 15 e BI 253 Runaway star from Tarantula Nebula of LMC 97 6 164 000 13 76 54 000 Spectroscopy SIMBAD 17 45 R136a8 in Tarantula Nebula of LMC 96 157 000 14 42 49 500 Evolution SIMBAD 24 46 Westerhout 49 15 in Westerhout 49 96 36 200 18 307 J band 43 700 Evolution SIMBAD 5 6 HD 38282 B in Tarantula Nebula of LMC 95 163 000 11 11 combined 47 000 Binary SIMBAD 47 23 HM 1 6 in HM 1 95 11 000 11 64 44 700 Evolution SIMBAD 26 48 NGC 3603 42 in HD 97950 of NGC 3603 95 25 000 12 86 50 000 Spectroscopy SIMBAD 18 21 R139 A in Tarantula Nebula of LMC 95 163 000 11 94 combined 35 000 Binary SIMBAD 7 8 BAT99 6 in NGC 1747 of LMC 94 165 000 11 95 56 000 Spectroscopy SIMBAD 7 19 Sk 66 172 in N64 of LMC 94 160 000 13 1 46 300 Spectroscopy SIMBAD 18 19 h ST2 22 in NGC 2044 of LMC 94 160 000 14 3 51 300 Evolution SIMBAD 28 49 VFTS 259 in Tarantula Nebula of LMC 94 164 000 13 65 37 600 Spectroscopy SIMBAD 11 8 VFTS 562 in Tarantula Nebula of LMC 94 164 000 13 66 42 200 Spectroscopy SIMBAD 11 8 VFTS 512 in Tarantula Nebula of LMC 93 164 000 14 28 47 300 Spectroscopy SIMBAD 11 8 HD 97950 A1b WR 43a B in HD 97950 of NGC 3603 92 24 800 11 18 combined 40 000 Binary SIMBAD 20 21 R136b in Tarantula Nebula of LMC 92 163 000 13 24 35 500 Evolution SIMBAD 24 8 VFTS 16 in Tarantula Nebula of LMC 91 6 164 000 13 55 50 600 Spectroscopy SIMBAD 17 8 HD 97950 A3 in HD 97950 of NGC 3603 91 24 800 12 95 50 000 Spectroscopy SIMBAD 18 21 NGC 346 W1 in NGC 346 of SMC 91 200 000 12 57 43 400 Evolution SIMBAD 28 50 R127 in NGC 2055 of LMC 90 160 000 10 15 10 000 27 000 Evolution SIMBAD 51 23 VFTS 333 in Tarantula Nebula of LMC 90 164 000 12 49 37 600 Spectroscopy SIMBAD 11 8 VFTS 267 in Tarantula Nebula of LMC 89 164 000 13 49 44 700 Spectroscopy SIMBAD 11 8 VFTS 64 in Tarantula Nebula of LMC 88 164 000 14 621 39 800 Spectroscopy SIMBAD 11 19 BAT99 80 A in NGC 2044 of LMC 87 165 000 13 combined 45 000 Spectroscopy SIMBAD 28 49 R140b in Tarantula Nebula of LMC 87 165 000 12 66 47 000 Spectroscopy SIMBAD 7 8 VFTS 542 in Tarantula Nebula of LMC 87 164 000 13 47 44 700 Spectroscopy SIMBAD 11 8 VFTS 599 in Tarantula Nebula of LMC 87 164 000 13 8 44 700 Spectroscopy SIMBAD 11 8 WR 89 in HM 1 87 11 000 11 02 39 800 Evolution SIMBAD 33 23 Arches F7 WR 102aj in Arches Cluster 86 3 25 000 15 74 J band 32 900 Spectroscopy SIMBAD 35 36 Sk 69 104 in NGC 1910 of LMC 86 160 000 12 1 39 900 Evolution SIMBAD 28 19 VFTS 1017 in Tarantula Nebula of LMC 86 164 000 14 5 50 100 Spectroscopy SIMBAD 11 8 LH 10 3061 in NGC 1763 of LMC 85 160 000 13 491 52 000 Spectroscopy SIMBAD 18 19 Sk 80 in NGC 346 of SMC 85 200 000 12 31 38 900 Evolution SIMBAD 28 52 VFTS 603 in Tarantula Nebula of LMC 85 164 000 13 99 42 200 Spectroscopy SIMBAD 11 8 Sk 70 91 in BSDL 1830 of LMC 84 09 165 000 12 78 48 900 Evolution SIMBAD 53 19 i R147 in Tarantula Nebula of LMC 84 164 000 12 993 47 300 Spectroscopy SIMBAD 11 54 HD 93250 A in Trumpler 16 of Carina Nebula 83 3 7 500 7 5 combined 46 000 Evolution SIMBAD 55 15 e Melnick 33Na A in Tarantula Nebula of LMC 83 163 000 13 79 combined 50 000 Evolution SIMBAD 56 57 WR 20a A in Westerlund 2 82 7 20 000 13 28 combined 43 000 Binary SIMBAD 58 TIC 276934932 A in NGC 2048 of LMC 82 160 000 14 05 combined 45 000 Spectroscopy SIMBAD 18 19 WR 20a B in Westerlund 2 81 9 20 000 13 28 combined 43 000 Binary SIMBAD 58 Trumpler 27 27 in Trumpler 27 81 3 900 13 31 37 000 Evolution SIMBAD 26 23 BAT99 96 in Tarantula Nebula of LMC 80 165 000 13 76 42 000 Spectroscopy SIMBAD 7 8 HD 15570 in IC 1805 of Heart Nebula 80 7 500 8 11 46 000 Spectroscopy SIMBAD 14 15 HD 38282 A in Tarantula Nebula of LMC 80 163 000 11 11 combined 47 000 Binary SIMBAD 47 23 HSH95 46 in Tarantula Nebula of LMC 80 163 000 14 56 47 500 Evolution SIMBAD 24 8 Arches F15 in Arches Cluster 79 7 25 000 16 12 J band 35 600 Spectroscopy SIMBAD 35 36 BI 237 in BSDL 2527 of LMC 79 66 165 000 13 83 51 300 Spectroscopy SIMBAD 53 19 j VFTS 94 in Tarantula Nebula of LMC 79 164 000 14 161 42 200 Spectroscopy SIMBAD 11 19 VFTS 151 in Tarantula Nebula of LMC 79 164 000 14 13 42 200 Spectroscopy SIMBAD 11 8 LH 41 32 in NGC 1910 of LMC 78 160 000 13 086 48 200 Evolution SIMBAD 28 19 Pismis 24 17 in Pismis 24 of NGC 6357 78 5 900 11 84 42 700 Spectroscopy SIMBAD 59 48 VFTS 404 in Tarantula Nebula of LMC 78 164 000 14 14 44 700 Spectroscopy SIMBAD 11 8 Westerhout 51 2 in Westerhout 51 77 20 000 13 68 J band 42 700 Evolution SIMBAD 12 BAT99 68 in BSDL 2505 of LMC 76 165 000 14 13 45 000 Spectroscopy SIMBAD 7 19 k HD 93632 in Collinder 228 of Carina Nebula 76 10 000 8 23 45 400 Evolution SIMBAD 26 15 NGC 346 W3 in NGC 346 of SMC 76 200 000 12 8 52 500 Evolution SIMBAD 28 50 VFTS 169 in Tarantula Nebula of LMC 76 164 000 14 437 47 300 Spectroscopy SIMBAD 11 19 VFTS 440 in Tarantula Nebula of LMC 76 164 000 12 046 39 800 Spectroscopy SIMBAD 11 19 AB1 in DEM S10 of SMC 75 197 000 15 238 79 000 Spectroscopy SIMBAD 60 50 l WR 22 A in Bochum 10 of Carina Nebula 75 8 300 6 42 combined 44 700 Evolution SIMBAD 33 15 m Pismis 24 1NE in Pismis 24 of NGC 6357 74 6 500 11 42 500 Binary SIMBAD 59 61 VFTS 608 in Tarantula Nebula of LMC 74 164 000 14 22 42 200 Spectroscopy SIMBAD 11 8 HSH95 31 in Tarantula Nebula of LMC 73 163 000 14 12 47 500 Evolution SIMBAD 24 8 Mercer 30 3 in Mercer 30 of Dragonfish Nebula 73 40 000 12 62 J band 39 300 Evolution SIMBAD 44 g Mercer 30 11 in Mercer 30 of Dragonfish Nebula 73 40 000 12 33 J band 36 800 Evolution SIMBAD 44 g VFTS 566 in Tarantula Nebula of LMC 73 164 000 14 05 44 700 Spectroscopy SIMBAD 11 8 LH 64 16 in NGC 2001 of LMC 72 160 000 13 666 50 900 Evolution SIMBAD 28 30 NGC 2044 W35 in NGC 2044 of LMC 72 160 000 14 1 48 200 Evolution SIMBAD 28 19 VFTS 216 in Tarantula Nebula of LMC 72 164 000 14 389 44 700 Spectroscopy SIMBAD 11 19 ST2 1 in NGC 2044 of LMC 71 160 000 14 3 44 100 Evolution SIMBAD 28 49 VFTS 3 in Tarantula Nebula of LMC 71 164 000 11 56 21 000 Spectroscopy SIMBAD 62 8 Arches F12 WR 102af in Arches Cluster 70 25 000 16 4 J band 36 900 Spectroscopy SIMBAD 35 36 HD 15629 in IC 1805 of Heart Nebula 70 7 500 8 42 45 900 Spectroscopy SIMBAD 14 15 HD 37974 in N135 of LMC 70 163 000 10 99 22 500 Spectroscopy SIMBAD 63 23 n HD 93129 Ab in Trumpler 14 of Carina Nebula 70 7 500 7 31 combined 44 000 Trinary SIMBAD 39 64 M33 X 7 B in Triangulum Galaxy 70 2 700 000 18 7 35 000 Binary SIMBAD 65 66 Sk 69 194 A in NGC 2033 of LMC 70 160 000 12 131 combined 45 000 Evolution SIMBAD 28 54 e VFTS 125 in Tarantula Nebula of LMC 69 6 164 000 16 6 55 200 Spectroscopy SIMBAD 17 49 HD 46150 in NGC 2244 of Rosette Nebula 69 5 200 6 73 44 000 Spectroscopy SIMBAD 18 15 HD 229059 in Berkeley 87 69 3 000 8 7 26 300 Evolution SIMBAD 26 15 ST2 3 in NGC 2044 of LMC 69 160 000 14 264 44 900 Evolution SIMBAD 28 19 ST2 32 in NGC 2044 of LMC 69 160 000 13 903 45 400 Evolution SIMBAD 28 19 W28 23 in NGC 2033 of LMC 69 160 000 13 702 51 300 Evolution SIMBAD 28 30 HD 93403 A in Trumpler 16 of Carina Nebula 68 5 10 400 8 27 combined 39 300 Binary SIMBAD 67 23 HD 93130 in Collinder 228 of Carina Nebula 68 10 000 8 04 39 900 Evolution SIMBAD 26 15 HM 1 8 in HM 1 68 11 000 12 52 46 100 Evolution SIMBAD 26 48 HSH95 47 in Tarantula Nebula of LMC 68 163 000 14 72 43 500 Evolution SIMBAD 24 8 HSH95 48 in Tarantula Nebula of LMC 68 163 000 14 75 46 500 Evolution SIMBAD 24 46 Westerhout 51 61 in Westerhout 51 68 20 000 18 16 J band 38 000 Evolution SIMBAD 12 6 BAT99 93 in Tarantula Nebula of LMC 67 165 000 13 446 45 000 Spectroscopy SIMBAD 7 19 Sk 69 200 in NGC 2033 of LMC 67 160 000 11 18 26 300 Evolution SIMBAD 28 19 Arches F18 in Arches Cluster 66 9 25 000 16 7 J band 36 900 Spectroscopy SIMBAD 35 36 Arches F4 WR 102al in Arches Cluster 66 4 25 000 15 63 J band 36 800 Spectroscopy SIMBAD 35 36 BAT99 59 A in NGC 2020 of LMC 66 165 000 13 186 combined 71 000 Spectroscopy SIMBAD 7 19 e BAT99 104 in Tarantula Nebula of LMC 66 165 000 12 5 63 000 Spectroscopy SIMBAD 7 19 HD 5980 B in NGC 346 of SMC 66 200 000 11 31 combined 45 000 Trinary SIMBAD 68 64 HD 190429 A near Barnard 146 66 7 800 6 63 combined 46 000 Binary SIMBAD 69 15 LH 31 1003 in NGC 1858 of LMC 66 160 000 13 186 41 900 Evolution SIMBAD 28 19 LH 114 7 in N70 of LMC 66 160 000 13 66 50 000 Spectroscopy SIMBAD 18 19 o Pismis 24 1SW in Pismis 24 of NGC 6357 66 6 500 11 1 40 000 Binary SIMBAD 59 61 BAT99 126 in NGC 2081 of LMC 65 165 000 13 166 71 000 Spectroscopy SIMBAD 7 19 HSH95 40 in Tarantula Nebula of LMC 65 163 000 14 56 47 500 Evolution SIMBAD 24 8 HSH95 58 in Tarantula Nebula of LMC 65 163 000 14 8 47 500 Evolution SIMBAD 24 8 HSH95 89 in Tarantula Nebula of LMC 65 163 000 14 76 44 000 Spectroscopy SIMBAD 46 VFTS 63 in Tarantula Nebula of LMC 65 164 000 14 4 42 200 Spectroscopy SIMBAD 11 49 VFTS 145 in Tarantula Nebula of LMC 65 164 000 14 3 39 800 Spectroscopy SIMBAD 11 8 VFTS 518 in Tarantula Nebula of LMC 65 164 000 15 11 44 700 Spectroscopy SIMBAD 11 8 Westerhout 49 8 in Westerhout 49 65 36 200 15 617 J band 40 700 Evolution SIMBAD 5 6 BD 43 3654 Runaway star from Cygnus OB2 64 6 5 400 10 06 40 400 Evolution SIMBAD 70 64 BAT99 129 A in DEM L294 of LMC 64 165 000 14 701 combined 79 000 Spectroscopy SIMBAD 7 19 p e HSH95 50 in Tarantula Nebula of LMC 64 163 000 14 65 47 000 Evolution SIMBAD 24 8 Sk 69 25 in NGC 1748 of LMC 64 160 000 11 886 43 600 Evolution SIMBAD 28 19 Trumpler 27 23 in Trumpler 27 64 3 900 10 09 27 500 Evolution SIMBAD 26 23 Westerhout 49 5 in Westerhout 49 64 36 200 15 623 J band 42 700 Evolution SIMBAD 5 6 HD 46223 in NGC 2244 of Rosette Nebula 63 5 200 7 28 46 000 Spectroscopy SIMBAD 18 15 HD 64568 in NGC 2467 of Puppis OB2 63 16 000 9 39 54 000 Spectroscopy SIMBAD 18 23 HD 303308 in Trumpler 16 of Carina Nebula 63 9 200 8 17 51 300 Evolution SIMBAD 26 23 HR 6187 A in NGC 6193 of Ara OB1 63 4 300 5 54 combined 46 500 Septenary SIMBAD 71 15 LH 10 3058 in NGC 1763 of LMC 63 160 000 14 089 54 000 Spectroscopy SIMBAD 18 19 ST5 71 in NGC 2074 of LMC 63 160 000 13 266 45 400 Evolution SIMBAD 28 19 AB9 in DEM S80 of SMC 62 197 000 15 431 100 000 Spectroscopy SIMBAD 60 50 q Brey 32 B in NGC 1966 of LMC 62 165 000 12 32 combined 43 600 Evolution SIMBAD 28 23 HD 93160 in Trumpler 14 of Carina Nebula 62 8 000 7 6 42 700 Evolution SIMBAD 26 15 HSH95 35 in Tarantula Nebula of LMC 62 163 000 14 43 47 500 Evolution SIMBAD 24 8 LH 41 1017 in NGC 1910 of LMC 62 160 000 12 266 42 700 Evolution SIMBAD 28 19 Mercer 30 6a A WR 46 4 A in Mercer 30 of Dragonfish Nebula 62 40 000 10 39 J band 29 900 Evolution SIMBAD 44 g e ST4 18 in NGC 2081 of LMC 62 160 000 13 639 44 800 Evolution SIMBAD 28 19 VFTS 664 in Tarantula Nebula of LMC 62 164 000 13 937 39 900 Spectroscopy SIMBAD 11 19 HD 229196 in Cygnus OB9 61 6 5 000 8 59 40 900 Evolution SIMBAD 70 48 AB8 B in NGC 602 of SMC 61 197 000 12 83 combined 45 000 Binary SIMBAD 68 72 BAT99 79 A in NGC 2044 of LMC 61 165 000 13 486 combined 42 000 Spectroscopy SIMBAD 7 19 e HD 5980 A in NGC 346 of SMC 61 200 000 11 31 combined 21 000 53 000 Trinary SIMBAD 68 64 LH 41 18 in NGC 1910 of LMC 61 160 000 12 586 38 500 Evolution SIMBAD 28 19 Mercer 30 9 A in Mercer 30 of Dragonfish Nebula 61 40 000 12 25 J band 34 500 Evolution SIMBAD 44 g e ST5 25 in NGC 2074 of LMC 61 160 000 13 551 48 600 Evolution SIMBAD 28 30 VFTS 422 in Tarantula Nebula of LMC 61 164 000 15 14 39 800 Spectroscopy SIMBAD 11 8 WR 102hb in Quintuplet cluster 61 26 000 13 9 J band 25 100 Evolution SIMBAD 73 74 Sk 67 166 in GKK A144 of LMC 60 68 160 000 12 22 41 800 Spectroscopy SIMBAD 53 19 r Sk 67 167 in GKK A144 of LMC 60 68 160 000 12 586 41 800 Spectroscopy SIMBAD 53 19 r Sk 71 46 in BSDL 2242 of LMC 60 68 160 000 13 241 41 800 Spectroscopy SIMBAD 53 19 s Brey 10 in NGC 1770 of LMC 60 165 000 12 69 117 000 Evolution SIMBAD 28 23 Brey 94 A in NGC 2081 of LMC 60 165 000 12 996 combined 83 000 Evolution SIMBAD 28 19 e Brey 95a A in NGC 2081 of LMC 60 165 000 12 2 combined 83 000 Evolution SIMBAD 28 75 e HSH95 55 in Tarantula Nebula of LMC 60 163 000 14 74 47 500 Evolution SIMBAD 24 8 Mercer 30 7 A WR 46 5 A in Mercer 30 of Dragonfish Nebula 60 40 000 11 516 J band 41 400 Evolution SIMBAD 44 g e R134 in Tarantula Nebula of LMC 60 164 000 12 75 39 800 Spectroscopy SIMBAD 11 8 R142 in Tarantula Nebula of LMC 60 164 000 11 82 18 000 Spectroscopy SIMBAD 62 8 R143 in Tarantula Nebula of LMC 60 160 000 12 014 18 000 36 000 Evolution SIMBAD 51 19 Sk 69 142a in NGC 1983 of LMC 60 160 000 11 093 34 000 Evolution SIMBAD 51 54 Sk 69 259 in NGC 2081 of LMC 60 160 000 11 93 23 000 Evolution SIMBAD 28 23 Var 83 in Triangulum Galaxy 60 3 000 000 16 027 18 000 37 000 Evolution SIMBAD 76 77 VFTS 430 in Tarantula Nebula of LMC 60 164 000 15 11 24 500 Spectroscopy SIMBAD 62 8 A few notable stars of mass less than 60 M are included for the purpose of comparison Star name Mass M Sun 1 Approx distancefrom earth ly Apparentvisible magnitude Effectivetemperature K Estimationmethod Link Referencez Puppis Naos in Vela R2 of Vela Molecular Ridge 56 1 1 080 2 25 40 000 Spectroscopy SIMBAD 69 15 t l Cephei Runaway star from Cepheus OB3 51 4 3 100 5 05 36 000 Spectroscopy SIMBAD 69 15 t Canis Majoris Aa in NGC 2362 50 5 120 4 89 32 000 Evolution SIMBAD 78 15 8 Muscae Ab in Centaurus OB1 44 7 400 5 53 combined 33 000 Evolution SIMBAD 79 15 e Orionis Alnilam in Orion OB1 of Orion complex 40 2 000 1 69 27 500 Evolution SIMBAD 80 15 82 Orionis A in Orion OB1 of Orion complex 39 1 500 5 02 34 900 Evolution SIMBAD 81 82 a Camelopardalis Runaway star from NGC 1502 37 6 6 000 4 29 29 000 Evolution SIMBAD 83 15 P Cygni in IC 4996 of Cygnus OB1 37 5 100 4 82 18 700 Spectroscopy SIMBAD 84 15 u z1 Scorpii in NGC 6231 of Scorpius OB1 36 8 210 4 705 17 200 Spectroscopy SIMBAD 37 85 z Orionis Aa Alnitak in Orion OB1 of Orion complex 33 1 260 2 08 29 500 Evolution SIMBAD 86 81 Orionis C1 in Trapezium Cluster of Orion complex 33 1 340 5 13 combined 39 000 Evolution SIMBAD 87 15 k Cassiopeiae in Cassiopeia OB14 33 4 000 4 16 23 500 Evolution SIMBAD 88 15 m Normae in NGC 6169 33 3 260 4 91 28 000 Spectroscopy SIMBAD 89 15 h Carinae B in Trumpler 16 of Carina Nebula 30 7 500 4 3 combined 37 200 Binary SIMBAD 90 43 g2 Velorum B in Vela OB2 28 5 1 230 1 83 combined 35 000 Evolution SIMBAD 91 15 l Orionis A Meissa in Collinder 69 of Orion complex 27 9 1 100 3 54 37 700 Spectroscopy SIMBAD 89 92 3 Persei Menkib in California Nebula of Perseus OB2 26 1 1 200 4 04 35 000 Evolution SIMBAD 83 15 WR 79a in NGC 6231 of Scorpius OB1 24 4 5 600 5 77 35 000 Spectroscopy SIMBAD 89 15 d Orionis Aa1 Mintaka in Orion OB1 of Orion complex 24 1 200 2 5 combined 29 500 Evolution SIMBAD 93 94 i Orionis Aa1 Hatysa in NGC 1980 of Orion complex 23 1 1 340 2 77 combined 32 500 Evolution SIMBAD 95 96 k Crucis in Jewel Box Cluster of Centaurus OB1 23 7 500 5 98 16 300 Evolution SIMBAD 97 64 WR 78 in NGC 6231 of Scorpius OB1 22 4 100 6 48 50 100 Spectroscopy SIMBAD 33 34 o2 Canis Majoris in Collinder 121 21 4 2 800 3 043 15 500 Evolution SIMBAD 89 15 b Orionis A Rigel in Orion OB1 of Orion complex 21 860 0 13 12 100 Evolution SIMBAD 98 15 h Canis Majoris Aludra in Collinder 121 21 2 000 2 45 15 000 Evolution SIMBAD 88 15 z Ophiuchi in Upper Scorpius subgroup of Scorpius OB2 20 2 370 2 569 34 000 Evolution SIMBAD 83 15 y Orionis in Orion OB1 of Orion complex 20 2 900 4 618 33 400 Evolution SIMBAD 99 100 s Orionis Aa in Orion OB1 of Orion complex 18 1 260 4 07 combined 35 000 Spectroscopy SIMBAD 101 102 m Columbae Runaway star from Trapezium Cluster 16 1 300 5 18 33 000 Spectroscopy SIMBAD 103 15 k Orionis Saiph in Orion OB1 of Orion complex 15 5 650 2 09 26 500 Evolution SIMBAD 104 15 s Cygni in Cygnus OB4 15 3 260 4 233 10 800 Evolution SIMBAD 105 106 8 Carinae A in IC 2602 of Scorpius OB2 14 9 460 2 76 combined 31 000 Evolution SIMBAD 89 107 82 Orionis B in Orion OB1 of Orion complex 14 8 1 500 6 38 29 300 Spectroscopy SIMBAD 108 z Persei in Perseus OB2 14 5 750 2 86 20 800 Evolution SIMBAD 104 15 s Orionis B in Orion OB1 of Orion complex 14 1 260 4 07 combined 31 000 Spectroscopy SIMBAD 101 102 b Canis Majoris Mirzam in Local Bubble of Scorpius OB2 13 5 490 1 985 23 200 Evolution SIMBAD 109 110 e Persei A in a Persei Cluster 13 5 640 2 88 combined 26 500 Evolution SIMBAD 111 112 i Orionis Aa2 in NGC 1980 of Orion complex 13 1 1 340 2 77 combined 27 000 Evolution SIMBAD 95 96 d Scorpii A Dschubba in Upper Scorpius subgroup of Scorpius OB2 13 440 2 307 combined 27 400 Evolution SIMBAD 113 114 s Orionis Ab in Orion OB1 of Orion complex 13 1 260 4 07 combined 29 000 Spectroscopy SIMBAD 101 102 8 Muscae Aa WR 48 in Centaurus OB1 11 5 7 400 5 53 combined 83 000 Spectroscopy SIMBAD 115 15 g2 Velorum A WR 11 in Vela OB2 9 1 230 1 83 combined 57 000 Spectroscopy SIMBAD 91 15 r Ophiuchi A in r Ophiuchi cloud complex of Scorpius OB2 8 7 360 4 63 combined 22 000 Evolution SIMBAD 89 15 g Orionis Bellatrix in Bellatrix Cluster of Orion complex 7 7 250 1 64 21 800 Evolution SIMBAD 116 15 a Scorpii B in Loop I Bubble of Scorpius OB2 7 2 550 5 5 18 500 Evolution SIMBAD 117 92 l Tauri A in Pisces Eridanus stellar stream 7 18 480 3 47 combined 18 700 Evolution SIMBAD 118 119 d Persei in a Persei Cluster 7 520 3 01 14 900 Evolution SIMBAD 89 107 ps Persei in a Persei Cluster 6 2 580 4 31 16 000 Evolution SIMBAD 89 15 a Pavonis Aa Peacock in Tucana Horologium association 5 91 180 1 94 17 700 Evolution SIMBAD 120 96 h Tauri A Alcyone in Pleiades 5 9 440 2 87 combined 12 300 Evolution SIMBAD 121 15 g Canis Majoris Muliphein in Collinder 121 5 6 440 4 1 13 600 Evolution SIMBAD 89 122 o Velorum in IC 2391 of Scorpius OB2 5 5 490 3 6 16 200 Evolution SIMBAD 123 107 o Aquarii in Pisces Eridanus stellar stream 4 2 440 4 71 13 500 Evolution SIMBAD 124 125 n Fornacis in Pisces Eridanus stellar stream 3 65 370 4 69 13 400 Evolution SIMBAD 126 15 f Eridani in Tucana Horologium association 3 55 150 3 55 13 700 Evolution SIMBAD 120 127 h Chamaeleontis in h Chamaeleontis moving group of Scorpius OB2 3 2 310 5 453 12 500 Evolution SIMBAD 128 64 e Chamaeleontis in e Chamaeleontis moving group of Scorpius OB2 2 87 360 4 91 10 900 Evolution SIMBAD 129 107 t1 Aquarii in Pisces Eridanus stellar stream 2 68 320 5 66 10 600 Evolution SIMBAD 130 131 e Hydri in Tucana Horologium association 2 64 150 4 12 11 000 Evolution SIMBAD 130 132 b1 Tucanae in Tucana Horologium association 2 5 140 4 37 10 600 Evolution SIMBAD 89 92 Sun in Solar System 1 0 0000158 26 744 5 772 Standard IAU 133 134 135 For some methods different determinations of chemical composition lead to different estimates of mass For a binary star it is possible to measure the individual masses of the two stars by studying their orbital motions using Kepler s laws of planetary motion The superwinds from massive stars are similar to the superwinds generated by asymptotic giant branch AGB stars red giants that form planetary nebulae These stars later remnants become the technically non stellar white dwarf cores of planetary nebulae For examples of stellar debris see hypernovae and supernova remnant a b c d e f g h i j k l m n o This is a binary system but the secondary is much less massive than the primary This unusual measurement was made by assuming the star was ejected from a three body encounter in NGC 3603 This assumption also means that the current star is the result of a merger between two original close binary components The mass is consistent with evolutionary mass for a star with the observed parameters a b c d e f Mercer 30 is an open cluster in Dragonfish Nebula N64 is an emission nebula in Large Magellanic Cloud BSDL 1830 is a star cluster in Large Magellanic Cloud BSDL 2527 is a star cluster in Large Magellanic Cloud BSDL 2505 is a star cluster in Large Magellanic Cloud DEM S10 is a H II region in Small Magellanic Cloud Bochum 10 is an open cluster in Carina Nebula N135 is an emission nebula in Large Magellanic Cloud N70 is an emission nebula in Large Magellanic Cloud DEM L294 is a H II region in Large Magellanic Cloud DEM S80 is a H II region in Small Magellanic Cloud a b GKK A144 is a stellar association in Large Magellanic Cloud BSDL 2242 is a star cluster in Large Magellanic Cloud Vela R2 is a OB association in Vela Molecular Ridge IC 4996 is an open cluster in Cygnus OB1 Black holes EditMain articles Black hole List of black holes and List of most massive black holes Black holes are the end point evolution of massive stars Technically they are not stars as they no longer generate heat and light via nuclear fusion in their cores Some black holes may have cosmological origins and would then never have been stars This is thought to be especially likely in the cases of the most massive black holes Stellar black holes are objects with approximately 4 15 M Intermediate mass black holes range from 100 to 10 000 M Supermassive black holes are in the range of millions or billions M See also EditHypergiant List of brightest stars List of brown dwarfs List of galaxies List of hottest stars List of largest cosmic structures List of largest nebulae List of largest known stars List of most luminous stars List of most massive black holes List of most massive neutron stars Lists of stars Luminous blue variable Supergiant Wolf Rayet starReferences Edit van Marle A J Owocki S P Shaviv N J March 2008 Continuum driven winds from super Eddington stars A tale of two limits First Stars III First Stars III Conference AIP Conference Proceedings AIP Conference Proceedings Vol 990 Santa Fe NM pp 250 253 arXiv 0708 4207 Bibcode 2008AIPC 990 250V doi 10 1063 1 2905555 ISSN 0094 243X S2CID 118364586 Maeder A Georgy C Meynet G Ekstrom S March 2012 On the Eddington limit and Wolf Rayet stars Astronomy amp Astrophysics 539 A110 arXiv 1201 5013 Bibcode 2012A amp A 539A 110M doi 10 1051 0004 6361 201118328 ISSN 0004 6361 S2CID 119230088 Banerjee Sambaran Kroupa Pavel Oh Seungkyung 21 October 2012 The emergence of super canonical stars in R136 type starburst clusters Super canonical stars in R136 Monthly Notices of the Royal Astronomical Society 426 2 1416 1426 arXiv 1208 0826 Bibcode 2012MNRAS 426 1416B doi 10 1111 j 1365 2966 2012 21672 x ISSN 0035 8711 S2CID 119202197 Ulmer Andrew Fitzpatrick Edward L September 1998 Revisiting the modified Eddington limit for massive stars The Astrophysical Journal 504 1 200 206 arXiv astro ph 9708264 Bibcode 1998ApJ 504 200U doi 10 1086 306048 ISSN 0004 637X S2CID 14916494 a b c d e f Wu Shi Wei Bik Arjan 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