# List of most massive stars

This is a list of the most massive stars that have been discovered, in solar mass units (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, composition, 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.

### 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. This obstruction leads to difficulties in determining the parameters needed to calculate the star's mass.
Both the obscuring clouds and the great distances also 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 for our telescopes to distinguish, each star possibly being massive in itself but not necessarily "supermassive" to either be on this list, or near the top of it. And certainly 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 clearly see inside the surrounding cloud, it is difficult to know what kind of object is actually generating the bright point of light seen from the Earth.
More globally, statistics on stellar populations seem to indicate that the upper mass limit is in the 100–200 solar mass range, so any mass estimate above this range is 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.
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. 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 infuses the adjacent volume of space with elements heavier than hydrogen or helium.
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. 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.
This list only concerns "living" stars – those which are still seen by Earth-based observers existing as active stars: Still engaged in interior nuclear fusion that generates heat and light. That is, the light now arriving at the Earth as images of the stars listed still shows them to internally generate new energy as of the time (in the distant past) that light now being received was emitted. The list specifically excludes both white dwarfs – former stars that are now seen to be "dead" but radiating residual heat – and black holes – fragmentary remains of exploded stars which have gravitationally collapsed, even though accretion disks surrounding those black holes might generate heat or light exterior to the star's remains (now inside the black hole), radiated by infalling matter (see § Black holes below).

### Mass limits

There are two related theoretical limits on how massive a star can possibly be: The accretion mass 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 already collected 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. Since their different compositions make them more transparent, Population II and Population III stars have higher and much higher mass limits, respectively.

#### Accretion limits

Astronomers have long hypothesized that as a protostar grows to a size beyond 120 M$_☉$, something drastic must happen. 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$_☉$.
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, on rare occasions, collide and merge when certain unusual circumstances hold that make a collision possible.

#### Eddington mass limit

Eddington's 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.

## List of the most massive known stars

Legend :
* Wolf–Rayet star
* Luminous blue variable
* O-type star
* B-type star
The following two lists show a few of the known stars, including the stars in open clusters, OB associations, and H II regions. 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 | Location | Mass (M$_☉$) | Approx. dist. (ly) | Spectral type | Appt. vis. mag. | Eff. temp. (K) | Mass est. method | Link |
| BAT99-98 | Tarantula Nebula | 226 | 165,000 | WN6 | 13.37 | 45,000 | spectroscopy | SIMBAD |
| R136a1 | Tarantula Nebula | 196+34 −27 | 163,000 | WN5h | 12.23 | 46,000 | evolution | SIMBAD |
| Melnick 42 | Tarantula Nebula | 189 | 163,000 | O2If* | 12.78 | 47,300 | spectroscopy | SIMBAD |
| VFTS 1022 | Tarantula Nebula | 178 | 164,000 | O3.5If*/WN7 | 13.47 | 42,200 | spectroscopy | SIMBAD |
| Westerhout 51-57 | Westerhout 51 | 160 | 20,000 | O4V | 16.66 J band | 42,700 | evolution | |
| R136a3 | Tarantula Nebula | 155 | 163,000 | WN5h | 12.97 | 50,000 | evolution | SIMBAD |
| VFTS 682 | Tarantula Nebula | 153 | 164,000 | WN5h | 16.08 | 52,200 | spectroscopy | SIMBAD |
| HD 15558 A | IC 1805 | ≥152±51 | 24,400 | O5.5III(f) | 7.87 combined | 39,500 | binary | SIMBAD |
| R136a2 | Tarantula Nebula | 151 | 163,000 | WN5h | 12.34 | 50,000 | evolution | SIMBAD |
| Westerhout 51-3 | Westerhout 51 | 148+105 −82 | 20,000 | O3-8V | 17.79 J band | 39,800 | evolution | SIMBAD |
| Melnick 34 A | Tarantula Nebula | 147±22 | 163,000 | WN5h | 13.09 combined | 53,000 | binary | SIMBAD |
| VFTS 482 | Tarantula Nebula | 145 | 164,000 | O3If*/WN6-A | 12.95 | 42,200 | spectroscopy | SIMBAD |
| R136c | Tarantula Nebula | 142 | 163,000 | WN5h | 13.43 | 51,000 | evolution | SIMBAD |
| VFTS 1021 | Tarantula Nebula | 141 | 164,000 | O4 If+ | 13.35 | 39,800 | spectroscopy | SIMBAD |
| LH 10-3209 A | NGC 1763 | 140 | 160,000 | O3III(f*) | 11.859 combined | 42,500 | spectroscopy | SIMBAD |
| Melnick 34 B | Tarantula Nebula | 136±20 | 163,000 | WN5h | 13.09 combined | 53,000 | binary | SIMBAD |
| Westerhout 51d | Westerhout 51 | 135 | 20,000 | | 15.11 J band | 42,700 | evolution | |
| VFTS 545 | Tarantula Nebula | 133 | 164,000 | O2If*/WN5 | 13.32 | 47,300 | spectroscopy | SIMBAD |
| HD 97950 B | WR 43b in HD 97950 | 132 | 24,800 | WN6h | 11.33 | 42,000 | spectroscopy | SIMBAD |
| HD 269810 | NGC 2029 | 130 | 163,000 | O2III(f*) | 12.22 | 52,500 | spectroscopy | SIMBAD |
| R136a7 | Tarantula Nebula | 127 | 163,000 | O3III(f*) | 13.97 | 54,000 | evolution | SIMBAD |
| WR 42e | HD 97950 | 123 | 25,000 | O3If*/WN6 | 14.53 | 43,000 | Ejection | SIMBAD |
| VFTS 506 | Tarantula Nebula | 122 | 164,000 | ON2V((n))((f*)) | 13.31 | 47,300 | spectroscopy | SIMBAD |
| HD 97950 A1a | WR 43a A in HD 97950 | 120 | 24,800 | WN6h | 11.18 combined | 42,000 | binary | SIMBAD |
| LSS 4067 | HM 1 | 120 | 11,000 | O4.5Ifpe | 11.44 | 40,000 | evolution | SIMBAD |
| WR 93 | Pismis 24 | 120 | 5,900 | WC7 | 10.68 | 71,000 | evolution | SIMBAD |
| Sk -69° 212 | NGC 2044 | 119 | 160,000 | O6If | 12.416 | 45,400 | evolution | SIMBAD |
| Sk -69° 249 A | NGC 2074 | 119 | 160,000 | O7If | 12.02 combined | 38,900 | evolution | SIMBAD |
| ST5-31 | NGC 2074 | 119 | 160,000 | O2-3(n)fp | 12.273 | 50,700 | evolution | SIMBAD |
| R136a5 | Tarantula Nebula | 116 | 157,000 | O2I(n)f* | 13.71 | 48,000 | evolution | SIMBAD |
| MSP 183 | Westerlund 2 | 115 | 20,000 | O3V(f) | 13.878 | 46,300 | spectroscopy | SIMBAD |
| WR 24 | Collinder 228 | 114 | 14,000 | WN6ha-w | 6.48 | 50,100 | evolution | SIMBAD |
| HD 97950 C1 | WR 43c A in HD 97950 | 113 | 24,800 | WN6h | 11.89 combined | 44,000 | spectroscopy | SIMBAD |
| Arches-F9 | WR 102ae in Arches Cluster | 111.3 | 25,000 | WN8-9h | 16.1 J band | 36,600 | spectroscopy | SIMBAD |
| Cygnus OB2 #12 A | Cygnus OB2 | 110 | 5,200 | B3–4 Ia+ | 11.702 combined | 13,700 | spectroscopy | SIMBAD |
| HD 93129 Aa | Trumpler 14 | 110 | 7,500 | O2If | 6.9 combined | 42,500 | trinary | SIMBAD |
| HSH95-36 | Tarantula Nebula | 110 | 163,000 | O2 If* | 14.41 | 49,500 | evolution | SIMBAD |
| R146 | Tarantula Nebula | 109 | 164,000 | WN4 | 13.11 | 63,000 | spectroscopy | SIMBAD |
| R136a4 | Tarantula Nebula | 108 | 157,000 | O3 V((f*))(n) | 13.41 | 50,000 | evolution | SIMBAD |
| VFTS 621 | Tarantula Nebula | 107 | 164,000 | O2V((f*))z | 15.39 | 54,000 | spectroscopy | SIMBAD |
| R136a6 | Tarantula Nebula | 105 | 157,000 | O2I(n)f*p | 13.35 | 52,000 | evolution | SIMBAD |
| Westerhout 49-3 | Westerhout 49 | 105 | 36,200 | O3-O7V | 16.689 J band | 40,700 | evolution | SIMBAD |
| WR 21a A | Runaway star from Westerlund 2 | 103.6 | 26,100 | O3/WN5ha | 12.661 combined | 45,000 | binary | SIMBAD |
| R99 | N44 | 103 | 164,000 | Ofpe/WN9 | 11.52 | 28,000 | spectroscopy | SIMBAD |
| Arches-F6 | WR 102ah in Arches Cluster | 101 | 25,000 | WN8-9h | 15.75 J band | 33,900 | spectroscopy | SIMBAD |
| Sk -65° 47 | NGC 1923 | 101 | 160,000 | O4If | 12.466 | 47,800 | evolution | SIMBAD |
| Arches-F1 | WR 102ad in Arches Cluster | 100.9 | 25,000 | WN8-9h | 16.3 J band | 33,200 | spectroscopy | SIMBAD |
| HD 37836 | Large Magellanic Cloud | 100 | 163,000 | B0Iae | 10.55 | 28,200 | | SIMBAD |
| Peony Star | WR 102ka in Peony Nebula | 100 | 26,000 | Ofpe/WN9 | 12.978 J band | 25,100 | spectroscopy | SIMBAD |
| VFTS 457 | Tarantula Nebula | 100 | 164,000 | O3.5If*/WN7 | 13.74 | 39,800 | spectroscopy | SIMBAD |
| η Carinae A | Trumpler 16 | 100 | 7,500 | LBV | 4.3 combined | 9,400–35,200 | spectroscopy | SIMBAD |
| Mercer 30-1 A | WR 46-3 A in Mercer 30 | 99 | 40,000 | | 10.33 J band | 32,200 | evolution | SIMBAD |
| Sk -68° 137 | Tarantula Nebula | 99 | 160,000 | | 13.346 | 50,000 | spectroscopy | SIMBAD |
| WR 25 A | Trumpler 16 | 98 | 6,500 | O2.5If* | 8.8 combined | 50,100 | evolution | SIMBAD |
| BI 253 | runaway star from Tarantula Nebula | 97.6 | 164,000 | O2V | 13.76 | 54,000 | spectroscopy | SIMBAD |
| R136a8 | Tarantula Nebula | 96 | 157,000 | O2–3V | 14.42 | 49,500 | evolution | SIMBAD |
| HD 38282 B | Tarantula Nebula | 95 | 163,000 | | 11.11 combined | 47,000 | binary | SIMBAD |
| HM 1-6 | HM 1 | 95 | 11,000 | | 11.64 | 44,700 | evolution | SIMBAD |
| NGC 3603-42 | HD 97950 | 95 | 25,000 | | 12.86 | 50,000 | spectroscopy | SIMBAD |
| R139 A | Tarantula Nebula | 95 | 163,000 | | 11.94 combined | 35,000 | binary | SIMBAD |
| BAT99-6 | NGC 1747 | 94 | 165,000 | | 11.95 | 56,000 | spectroscopy | SIMBAD |
| Sk -66° 172 | N64 | 94 | 160,000 | | 13.1 | 46,300 | spectroscopy | SIMBAD |
| ST2-22 | NGC 2044 | 94 | 160,000 | | 14.3 | 51,300 | evolution | SIMBAD |
| VFTS 259 | Tarantula Nebula | 94 | 164,000 | | 13.65 | 37,600 | spectroscopy | SIMBAD |
| VFTS 562 | Tarantula Nebula | 94 | 164,000 | | 13.66 | 42,200 | spectroscopy | SIMBAD |
| VFTS 512 | Tarantula Nebula | 93 | 164,000 | | 14.28 | 47,300 | spectroscopy | SIMBAD |
| HD 97950 A1b | WR 43a B in HD 97950 | 92 | 24,800 | WN6h | 11.18 combined | 40,000 | binary | SIMBAD |
| R136b | Tarantula Nebula | 92 | 163,000 | | 13.24 | 35,500 | evolution | SIMBAD |
| VFTS 16 | Tarantula Nebula | 91.6 | 164,000 | | 13.55 | 50,600 | spectroscopy | SIMBAD |
| HD 97950 A3 | HD 97950 | 91 | 24,800 | | 12.95 | 50,000 | spectroscopy | SIMBAD |
| NGC 346-W1 | NGC 346 | 91 | 200,000 | | 12.57 | 43,400 | evolution | SIMBAD |
| Westerhout 49-2 | Westerhout 49 | 90–240, 250±120 | 36,200 | | 18.246 J band | 35,500 | spectroscopy | SIMBAD |
| R127 | NGC 2055 | 90 | 160,000 | | 10.15 | 10,000–27,000 | evolution | SIMBAD |
| VFTS 333 | Tarantula Nebula | 90 | 164,000 | | 12.49 | 37,600 | spectroscopy | SIMBAD |
| VFTS 267 | Tarantula Nebula | 89 | 164,000 | | 13.49 | 44,700 | spectroscopy | SIMBAD |
| VFTS 64 | Tarantula Nebula | 88 | 164,000 | | 14.621 | 39,800 | spectroscopy | SIMBAD |
| BAT99-80 A | NGC 2044 | 87 | 165,000 | | 13 combined | 45,000 | spectroscopy | SIMBAD |
| R140b | Tarantula Nebula | 87 | 165,000 | | 12.66 | 47,000 | spectroscopy | SIMBAD |
| VFTS 542 | Tarantula Nebula | 87 | 164,000 | | 13.47 | 44,700 | spectroscopy | SIMBAD |
| VFTS 599 | Tarantula Nebula | 87 | 164,000 | | 13.8 | 44,700 | spectroscopy | SIMBAD |
| WR 89 | HM 1 | 87 | 11,000 | | 11.02 | 39,800 | evolution | SIMBAD |
| Arches-F7 | WR 102aj in Arches Cluster | 86.3 | 25,000 | | 15.74 J band | 32,900 | spectroscopy | SIMBAD |
| Sk -69° 104 | NGC 1910 | 86 | 160,000 | | 12.1 | 39,900 | evolution | SIMBAD |
| VFTS 1017 | Tarantula Nebula | 86 | 164,000 | | 14.5 | 50,100 | spectroscopy | SIMBAD |
| LH 10-3061 | NGC 1763 | 85 | 160,000 | | 13.491 | 52,000 | spectroscopy | SIMBAD |
| Sk 80 | NGC 346 | 85 | 200,000 | | 12.31 | 38,900 | evolution | SIMBAD |
| VFTS 603 | Tarantula Nebula | 85 | 164,000 | | 13.99 | 42,200 | spectroscopy | SIMBAD |
| Sk -70° 91 | BSDL 1830 | 84.09 | 165,000 | | 12.78 | 48,900 | evolution | SIMBAD |
| R147 | Tarantula Nebula | 84 | 164,000 | | 12.993 | 47,300 | spectroscopy | SIMBAD |
| HD 93250 A | Trumpler 16 | 83.3 | 7,500 | | 7.5 combined | 46,000 | evolution | SIMBAD |
| Melnick 33Na A | Tarantula Nebula | 83 | 163,000 | | 13.79 combined | 50,000 | evolution | SIMBAD |
| WR 20a A | Westerlund 2 | 82.7 | 20,000 | | 13.28 combined | 43,000 | binary | SIMBAD |
| TIC 276934932 A | NGC 2048 | 82 | 160,000 | | 14.05 combined | 45,000 | spectroscopy | SIMBAD |
| WR 20a B | Westerlund 2 | 81.9 | 20,000 | | 13.28 combined | 43,000 | binary | SIMBAD |
| Trumpler 27-27 | Trumpler 27 | 81 | 3,900 | | 13.31 | 37,000 | evolution | SIMBAD |
| BAT99-96 | Tarantula Nebula | 80 | 165,000 | | 13.76 | 42,000 | spectroscopy | SIMBAD |
| HD 15570 | IC 1805 | 80 | 7,500 | | 8.11 | 46,000 | spectroscopy | SIMBAD |
| HD 38282 A | Tarantula Nebula | 80 | 163,000 | | 11.11 combined | 47,000 | binary | SIMBAD |
| HSH95-46 | Tarantula Nebula | 80 | 163,000 | | 14.56 | 47,500 | evolution | SIMBAD |
| Arches-F15 | Arches Cluster | 79.7 | 25,000 | | 16.12 J band | 35,600 | spectroscopy | SIMBAD |
| BI 237 | BSDL 2527 | 79.66 | 165,000 | | 13.83 | 51,300 | spectroscopy | SIMBAD |
| VFTS 94 | Tarantula Nebula | 79 | 164,000 | | 14.161 | 42,200 | spectroscopy | SIMBAD |
| VFTS 151 | Tarantula Nebula | 79 | 164,000 | | 14.13 | 42,200 | spectroscopy | SIMBAD |
| LH 41-32 | NGC 1910 | 78 | 160,000 | | 13.086 | 48,200 | evolution | SIMBAD |
| Pismis 24-17 | Pismis 24 | 78 | 5,900 | | 11.84 | 42,700 | spectroscopy | SIMBAD |
| VFTS 404 | Tarantula Nebula | 78 | 164,000 | | 14.14 | 44,700 | spectroscopy | SIMBAD |
| Westerhout 51-2 | Westerhout 51 | 77+26 −22 | 20,000 | | 13.68 J band | 42,700 | evolution | SIMBAD |
| BAT99-68 | BSDL 2505 | 76 | 165,000 | | 14.13 | 45,000 | spectroscopy | SIMBAD |
| HD 93632 | Collinder 228 | 76 | 10,000 | | 8.23 | 45,400 | evolution | SIMBAD |
| NGC 346-W3 | NGC 346 | 76 | 200,000 | | 12.8 | 52,500 | evolution | SIMBAD |
| VFTS 169 | Tarantula Nebula | 76 | 164,000 | | 14.437 | 47,300 | spectroscopy | SIMBAD |
| VFTS 440 | Tarantula Nebula | 76 | 164,000 | | 12.046 | 39,800 | spectroscopy | SIMBAD |
| AB1 | DEM S10 | 75 | 197,000 | | 15.238 | 79,000 | spectroscopy | SIMBAD |
| WR 22 A | Bochum 10 | 75 | 8,300 | | 6.42 combined | 44,700 | evolution | SIMBAD |
| Pismis 24-1NE | Pismis 24 | 74 | 6,500 | | 11 | 42,500 | binary | SIMBAD |
| VFTS 608 | Tarantula Nebula | 74 | 164,000 | | 14.22 | 42,200 | spectroscopy | SIMBAD |
| HSH95-31 | Tarantula Nebula | 73 | 163,000 | | 14.12 | 47,500 | evolution | SIMBAD |
| Mercer 30-3 | Mercer 30 | 73 | 40,000 | | 12.62 J band | 39,300 | evolution | SIMBAD |
| Mercer 30-11 | Mercer 30 | 73 | 40,000 | | 12.33 J band | 36,800 | evolution | SIMBAD |
| VFTS 566 | Tarantula Nebula | 73 | 164,000 | | 14.05 | 44,700 | spectroscopy | SIMBAD |
| LH 64-16 | NGC 2001 | 72 | 160,000 | | 13.666 | 50,900 | evolution | SIMBAD |
| NGC 2044-W35 | NGC 2044 | 72 | 160,000 | | 14.1 | 48,200 | evolution | SIMBAD |
| VFTS 216 | Tarantula Nebula | 72 | 164,000 | | 14.389 | 44,700 | spectroscopy | SIMBAD |
| ST2-1 | NGC 2044 | 71 | 160,000 | | 14.3 | 44,100 | evolution | SIMBAD |
| VFTS 3 | Tarantula Nebula | 71 | 164,000 | | 11.56 | 21,000 | spectroscopy | SIMBAD |
| Arches-F12 | WR 102af in Arches Cluster | 70 | 25,000 | | 16.4 J band | 36,900 | spectroscopy | SIMBAD |
| HD 15629 | IC 1805 | 70 | 7,500 | | 8.42 | 45,900 | spectroscopy | SIMBAD |
| HD 37974 | N135 | 70 | 163,000 | | 10.99 | 22,500 | spectroscopy | SIMBAD |
| HD 93129 Ab | Trumpler 14 | 70 | 7,500 | | 7.31 combined | 44,000 | trinary | SIMBAD |
| M33 X-7 B | Triangulum Galaxy | 70 | 2,700,000 | | 18.7 | 35,000 | binary | SIMBAD |
| Sk -69° 194 A | NGC 2033 | 70 | 160,000 | | 12.131 combined | 45,000 | evolution | SIMBAD |
| VFTS 125 | Tarantula Nebula | 69.6 | 164,000 | | 16.6 | 55,200 | spectroscopy | SIMBAD |
| HD 46150 | NGC 2244 | 69 | 5,200 | | 6.73 | 44,000 | spectroscopy | SIMBAD |
| HD 229059 | Berkeley 87 | 69 | 3,000 | | 8.7 | 26,300 | evolution | SIMBAD |
| ST2-3 | NGC 2044 of LMC | 69 | 160,000 | | 14.264 | 44,900 | evolution | SIMBAD |
| ST2-32 | NGC 2044 | 69 | 160,000 | | 13.903 | 45,400 | evolution | SIMBAD |
| W28-23 | NGC 2033 | 69 | 160,000 | | 13.702 | 51,300 | evolution | SIMBAD |
| HD 93403 A | Trumpler 16 | 68.5 | 10,400 | | 8.27 combined | 39,300 | binary | SIMBAD |
| HD 93130 | Collinder 228 | 68 | 10,000 | O7II(f) | 8.04 | 39,900 | evolution | SIMBAD |
| HM 1-8 | HM 1 | 68 | 11,000 | | 12.52 | 46,100 | evolution | SIMBAD |
| HSH95-47 | Tarantula Nebula | 68 | 163,000 | | 14.72 | 43,500 | evolution | SIMBAD |
| HSH95-48 | Tarantula Nebula | 68 | 163,000 | | 14.75 | 46,500 | evolution | SIMBAD |
| Westerhout 51-61 | Westerhout 51 | 68 | 20,000 | | 18.16 J band | 38,000 | evolution | SIMBAD |
| BAT99-93 | Tarantula Nebula | 67 | 165,000 | | 13.446 | 45,000 | spectroscopy | SIMBAD |
| Sk -69° 200 | NGC 2033 | 67 | 160,000 | | 11.18 | 26,300 | evolution | SIMBAD |
| Arches-F18 | Arches Cluster | 66.9 | 25,000 | | 16.7 J band | 36,900 | spectroscopy | SIMBAD |
| Arches-F4 | WR 102al in Arches Cluster | 66.4 | 25,000 | | 15.63 J band | 36,800 | spectroscopy | SIMBAD |
| BAT99-59 A | NGC 2020 | 66 | 165,000 | | 13.186 combined | 71,000 | spectroscopy | SIMBAD |
| BAT99-104 | Tarantula Nebula | 66 | 165,000 | | 12.5 | 63,000 | spectroscopy | SIMBAD |
| HD 5980 B | NGC 346 | 66 | 200,000 | | 11.31 combined | 45,000 | trinary | SIMBAD |
| HD 190429 A | near Barnard 146 | 66 | 7,800 | | 6.63 combined | 46,000 | binary | SIMBAD |
| LH 31-1003 | NGC 1858 | 66 | 160,000 | | 13.186 | 41,900 | evolution | SIMBAD |
| LH 114-7 | N70 | 66 | 160,000 | | 13.66 | 50,000 | spectroscopy | SIMBAD |
| Pismis 24-1SW | Pismis 24 | 66 | 6,500 | | 11.1 | 40,000 | binary | SIMBAD |
| BAT99-126 | NGC 2081 | 65 | 165,000 | | 13.166 | 71,000 | spectroscopy | SIMBAD |
| HSH95-40 | Tarantula Nebula | 65 | 163,000 | | 14.56 | 47,500 | evolution | SIMBAD |
| HSH95-58 | Tarantula Nebula | 65 | 163,000 | | 14.8 | 47,500 | evolution | SIMBAD |
| HSH95-89 | Tarantula Nebula | 65 | 163,000 | | 14.76 | 44,000 | spectroscopy | SIMBAD |
| VFTS 63 | Tarantula Nebula | 65 | 164,000 | | 14.4 | 42,200 | spectroscopy | SIMBAD |
| VFTS 145 | Tarantula Nebula | 65 | 164,000 | | 14.3 | 39,800 | spectroscopy | SIMBAD |
| VFTS 518 | Tarantula Nebula | 65 | 164,000 | | 15.11 | 44,700 | spectroscopy | SIMBAD |
| Westerhout 49-8 | Westerhout 49 | 65 | 36,200 | | 15.617 J band | 40,700 | evolution | SIMBAD |
| BD+43° 3654 | Runaway star from Cygnus OB2 | 64.6 | 5,400 | | 10.06 | 40,400 | evolution | SIMBAD |
| BAT99-129 A | DEM L294 | 64 | 165,000 | | 14.701 combined | 79,000 | spectroscopy | SIMBAD |
| HSH95-50 | Tarantula Nebula | 64 | 163,000 | | 14.65 | 47,000 | evolution | SIMBAD |
| Sk -69° 25 | NGC 1748 | 64 | 160,000 | | 11.886 | 43,600 | evolution | SIMBAD |
| Trumpler 27-23 | Trumpler 27 | 64 | 3,900 | | 10.09 | 27,500 | evolution | SIMBAD |
| Westerhout 49-5 | Westerhout 49 | 64 | 36,200 | | 15.623 J band | 42,700 | evolution | SIMBAD |
| HD 46223 | NGC 2244 | 63 | 5,200 | | 7.28 | 46,000 | spectroscopy | SIMBAD |
| HD 64568 | NGC 2467 | 63 | 16,000 | | 9.39 | 54,000 | spectroscopy | SIMBAD |
| HD 303308 | Trumpler 16 | 63 | 9,200 | | 8.17 | 51,300 | evolution | SIMBAD |
| HR 6187 A | NGC 6193 | 63 | 4,300 | | 5.54 combined | 46,500 | Septenary | SIMBAD |
| LH 10-3058 | NGC 1763 | 63 | 160,000 | | 14.089 | 54,000 | spectroscopy | SIMBAD |
| ST5-71 | NGC 2074 | 63 | 160,000 | | 13.266 | 45,400 | evolution | SIMBAD |
| AB9 | DEM S80 | 62 | 197,000 | | 15.431 | 100,000 | spectroscopy | SIMBAD |
| Brey 32 B | NGC 1966 | 62 | 165,000 | | 12.32 combined | 43,600 | evolution | SIMBAD |
| HD 93160 | Trumpler 14 | 62 | 8,000 | | 7.6 | 42,700 | evolution | SIMBAD |
| HSH95-35 | Tarantula Nebula | 62 | 163,000 | | 14.43 | 47,500 | evolution | SIMBAD |
| LH 41-1017 | NGC 1910 | 62 | 160,000 | | 12.266 | 42,700 | evolution | SIMBAD |
| Mercer 30-6a A | WR 46-4 A in Mercer 30 | 62 | 40,000 | | 10.39 J band | 29,900 | evolution | SIMBAD |
| ST4-18 | NGC 2081 | 62 | 160,000 | | 13.639 | 44,800 | evolution | SIMBAD |
| VFTS 664 | Tarantula Nebula | 62 | 164,000 | | 13.937 | 39,900 | spectroscopy | SIMBAD |
| HD 229196 | Cygnus OB9 | 61.6 | 5,000 | | 8.59 | 40,900 | evolution | SIMBAD |
| AB8 B | NGC 602 | 61 | 197,000 | O4V | 12.83 combined | 45,000 | binary | SIMBAD |
| BAT99-79 A | NGC 2044 | 61 | 165,000 | | 13.486 combined | 42,000 | spectroscopy | SIMBAD |
| HD 5980 A | NGC 346 | 61 | 200,000 | | 11.31 combined | 21,000–53,000 | trinary | SIMBAD |
| LH 41-18 | NGC 1910 | 61 | 160,000 | | 12.586 | 38,500 | evolution | SIMBAD |
| Mercer 30-9 A | Mercer 30 | 61 | 40,000 | | 12.25 J band | 34,500 | evolution | SIMBAD |
| ST5-25 | NGC 2074 | 61 | 160,000 | | 13.551 | 48,600 | evolution | SIMBAD |
| VFTS 422 | Tarantula Nebula | 61 | 164,000 | | 15.14 | 39,800 | spectroscopy | SIMBAD |
| WR 102hb | Quintuplet cluster | 61 | 26,000 | | 13.9 J band | 25,100 | evolution | SIMBAD |
| Sk -67° 166 | GKK-A144 | 60.68 | 160,000 | | 12.22 | 41,800 | spectroscopy | SIMBAD |
| Sk -67° 167 | GKK-A144 | 60.68 | 160,000 | | 12.586 | 41,800 | spectroscopy | SIMBAD |
| Sk -71° 46 | BSDL 2242 | 60.68 | 160,000 | | 13.241 | 41,800 | spectroscopy | SIMBAD |
| Brey 10 | NGC 1770 | 60 | 165,000 | | 12.69 | 117,000 | evolution | SIMBAD |
| Brey 94 A | NGC 2081 | 60 | 165,000 | | 12.996 combined | 83,000 | evolution | SIMBAD |
| Brey 95a A | NGC 2081 | 60 | 165,000 | | 12.2 combined | 83,000 | evolution | SIMBAD |
| HSH95-55 | Tarantula Nebula | 60 | 163,000 | | 14.74 | 47,500 | evolution | SIMBAD |
| Mercer 30-7 A | WR 46-5 A in Mercer 30 | 60 | 40,000 | | 11.516 J band | 41,400 | evolution | SIMBAD |
| R134 | Tarantula Nebula | 60 | 164,000 | | 12.75 | 39,800 | spectroscopy | SIMBAD |
| R142 | Tarantula Nebula | 60 | 164,000 | | 11.82 | 18,000 | spectroscopy | SIMBAD |
| R143 | Tarantula Nebula | 60 | 160,000 | | 12.014 | 18,000–36,000 | evolution | SIMBAD |
| Sk -69° 142a | NGC 1983 | 60 | 160,000 | | 11.093 | 34,000 | evolution | SIMBAD |
| Sk -69° 259 | NGC 2081 | 60 | 160,000 | | 11.93 | 23,000 | evolution | SIMBAD |
| Var 83 | Triangulum Galaxy | 60 | 3,000,000 | | 16.027 | 18,000–37,000 | evolution | SIMBAD |
| VFTS 430 | Tarantula Nebula | 60 | 164,000 | | 15.11 | 24,500 | spectroscopy | SIMBAD |
A few notable large stars with masses less than 60 M$_☉$ are shown in the table below for the purpose of comparison, ending with the Sun, which is very close, but would otherwise be too small to be included in the list. At present, all the listed stars are naked-eye visible and relatively nearby.
| Star name | Location | Mass (M$_☉$, Sun = 1) | Approx. dist. (ly) | Appt. vis. mag. | Eff. temp. (K) | Mass est. method | Link |
| λ Cephei | Runaway star from Cepheus OB3 | 51.4 | 3,100 | 5.05 | 36,000 | spectroscopy | SIMBAD |
| τ Canis Majoris Aa | NGC 2362 | 50 | 5,120 | 4.89 | 32,000 | evolution | SIMBAD |
| θ Muscae Ab | Centaurus OB1 | 44 | 7,400 | 5.53 combined | 33,000 | evolution | SIMBAD |
| ε Orionis | Alnilam in Orion OB1 of Orion complex | 40 | 1,180 | 1.69 | 27,500 | evolution | SIMBAD |
| θ$^2$ Orionis A | Orion OB1 of Orion complex | 39 | 1,500 | 5.02 | 34,900 | evolution | SIMBAD |
| α Camelopardalis | Runaway star from NGC 1502 | 37.6 | 6,000 | 4.29 | 29,000 | evolution | SIMBAD |
| P Cygni | IC 4996 of Cygnus OB1 | 37 | 5,100 | 4.82 | 18,700 | spectroscopy | SIMBAD |
| ζ$^1$ Scorpii | NGC 6231 of Scorpius OB1 | 36 - 53 | 8,210 | 4.705 | 17,200 | spectroscopy | SIMBAD |
| ζ Orionis Aa | Alnitak in Orion OB1 of Orion complex | 33 | 1,260 | 2.08 | 29,500 | evolution | SIMBAD |
| θ$^1$ Orionis C1 | Trapezium Cluster of Orion complex | 33 | 1,340 | 5.13 combined | 39,000 | evolution | SIMBAD |
| κ Cassiopeiae | Cassiopeia OB14 | 33 | 4,000 | 4.16 | 23,500 | evolution | SIMBAD |
| μ Normae | NGC 6169 | 33 | 3,260 | 4.91 | 28,000 | spectroscopy | SIMBAD |
| η Carinae B | Trumpler 16 of Carina Nebula | 30 | 7,500 | 4.3 combined | 37,200 | binary | SIMBAD |
| γ$^2$ Velorum B | Vela OB2 | 28.5 | 1,230 | 1.83 combined | 35,000 | evolution | SIMBAD |
| Meissa A | In Collinder 69 of Orion complex | 27.9 | 1,300 | 3.54 | 37,700 | spectroscopy | SIMBAD |
| ξ Persei | Menkib in California Nebula of Perseus OB2 | 26.1 | 1,200 | 4.04 | 35,000 | evolution | SIMBAD |
| ζ Puppis | Naos in Vela R2 of Vela Molecular Ridge | 25.3±5.3 | 1,080 | 2.25 | 40,000 | empirical | SIMBAD |
| WR 79a | NGC 6231 of Scorpius OB1 | 24.4 | 5,600 | 5.77 | 35,000 | spectroscopy | SIMBAD |
| Mintaka Aa1 | In Orion OB1 of Orion complex | 24 | 1,200 | 2.5 combined | 29,500 | evolution | SIMBAD |
| ι Orionis Aa1 | Hatysa in NGC 1980 of Orion complex | 23.1 | 1,340 | 2.77 combined | 32,500 | evolution | SIMBAD |
| κ Crucis | Jewel Box Cluster of Centaurus OB1 | 23 | 7,500 | 5.98 | 16,300 | evolution | SIMBAD |
| WR 78 | NGC 6231 of Scorpius OB1 | 22 | 4,100 | 6.48 | 50,100 | spectroscopy | SIMBAD |
| ο$^2$ Canis Majoris | Field star | 21.4 | 2,800 | 3.043 | 15,500 | evolution | SIMBAD |
| Rigel A | In Orion OB1 of Orion complex | 21 | 860 | 0.13 | 12,100 | evolution | SIMBAD |
| ζ Ophiuchi | Upper Scorpius subgroup of Scorpius OB2 | 20.2 | 370 | 2.569 | 34,000 | evolution | SIMBAD |
| υ Orionis | Orion OB1 of Orion complex | 20 | 2,900 | 4.618 | 33,400 | evolution | SIMBAD |
| σ Orionis Aa | Orion OB1 of Orion complex | 18 | 1,260 | 4.07 combined | 35,000 | spectroscopy | SIMBAD |
| μ Columbae | Runaway star from Trapezium Cluster | 16 | 1,300 | 5.18 | 33,000 | spectroscopy | SIMBAD |
| Saiph | In Orion OB1 of Orion complex | 15.5 | 650 | 2.09 | 26,500 | evolution | SIMBAD |
| σ Cygni | Cygnus OB4 | 15 | 3,260 | 4.233 | 10,800 | evolution | SIMBAD |
| θ Carinae A | IC 2602 of Scorpius OB2 | 14.9 | 460 | 2.76 combined | 31,000 | evolution | SIMBAD |
| θ$^2$ Orionis B | Orion OB1 of Orion complex | 14.8 | 1,500 | 6.38 | 29,300 | spectroscopy | SIMBAD |
| ζ Persei | Perseus OB2 | 14.5 | 750 | 2.86 | 20,800 | evolution | SIMBAD |
| σ Orionis B | Orion OB1 of Orion complex | 14 | 1,260 | 4.07 combined | 31,000 | spectroscopy | SIMBAD |
| β Canis Majoris | Mirzam in Local Bubble of Scorpius OB2 | 13.5 | 490 | 1.985 | 23,200 | evolution | SIMBAD |
| ε Persei A | α Persei Cluster | 13.5 | 640 | 2.88 combined | 26,500 | evolution | SIMBAD |
| ι Orionis Aa2 | NGC 1980 of Orion complex | 13.1 | 1,340 | 2.77 combined | 27,000 | evolution | SIMBAD |
| δ Scorpii A | Dschubba in Upper Scorpius subgroup of Scorpius OB2 | 13 | 440 | 2.307 combined | 27,400 | evolution | SIMBAD |
| σ Orionis Ab | Orion OB1 of Orion complex | 13 | 1,260 | 4.07 combined | 29,000 | spectroscopy | SIMBAD |
| θ Muscae Aa | WR 48 in Centaurus OB1 | 11.5 | 7,400 | 5.53 combined | 83,000 | spectroscopy | SIMBAD |
| γ$^2$ Velorum A | WR 11 in Vela OB2 | 9 | 1,230 | 1.83 combined | 57,000 | spectroscopy | SIMBAD |
| ρ Ophiuchi A | ρ Ophiuchi cloud complex of Scorpius OB2 | 8.7 | 360 | 4.63 combined | 22,000 | evolution | SIMBAD |
| Bellatrix | In Bellatrix Cluster of Orion complex | 7.7 | 250 | 1.64 | 21,800 | evolution | SIMBAD |
| Antares B | Loop I Bubble of Scorpius OB2 | 7.2 | 550 | 5.5 | 18,500 | evolution | SIMBAD |
| λ Tauri A | Pisces-Eridanus stellar stream | 7.18 | 480 | 3.47 combined | 18,700 | evolution | SIMBAD |
| δ Persei | α Persei Cluster | 7 | 520 | 3.01 | 14,900 | evolution | SIMBAD |
| ψ Persei | α Persei Cluster | 6.2 | 580 | 4.31 | 16,000 | evolution | SIMBAD |
| α Pavonis Aa | Peacock in Tucana-Horologium association | 5.91 | 180 | 1.94 | 17,700 | evolution | SIMBAD |
| Alcyone | In Pleiades | 5.9 | 440 | 2.87 combined | 12,300 | evolution | SIMBAD |
| γ Canis Majoris | Muliphein in Collinder 121 | 5.6 | 440 | 4.1 | 13,600 | evolution | SIMBAD |
| η Canis Majoris | Aludra in Collinder 121 | 5.5 or 9.5 | 2,000 | 2.45 | 15,000 | SED modelling / spectroscopy | SIMBAD |
| ο Velorum | IC 2391 of Scorpius OB2 | 5.5 | 490 | 3.6 | 16,200 | evolution | SIMBAD |
| ο Aquarii | Pisces-Eridanus stellar stream | 4.2 | 440 | 4.71 | 13,500 | evolution | SIMBAD |
| ν Fornacis | Pisces-Eridanus stellar stream | 3.65 | 370 | 4.69 | 13,400 | evolution | SIMBAD |
| φ Eridani | Tucana-Horologium association | 3.55 | 150 | 3.55 | 13,700 | evolution | SIMBAD |
| η Chamaeleontis | η Chamaeleontis moving group of Scorpius OB2 | 3.2 | 310 | 5.453 | 12,500 | evolution | SIMBAD |
| ε Chamaeleontis | ε Chamaeleontis moving group of Scorpius OB2 | 2.87 | 360 | 4.91 | 10,900 | evolution | SIMBAD |
| τ$^1$ Aquarii | Pisces-Eridanus stellar stream | 2.68 | 320 | 5.66 | 10,600 | evolution | SIMBAD |
| ε Hydri | Tucana-Horologium association | 2.64 | 150 | 4.12 | 11,000 | evolution | SIMBAD |
| β$^1$ Tucanae | Tucana-Horologium association | 2.5 | 140 | 4.37 | 10,600 | evolution | SIMBAD |
| Sun | Solar System | 1 | 0.0000158 | −26.744 | 5,772 | standard | IAU |
* ↑ For some methods, for any one temperature or brightness, different chemical composition indicates a different estimate for stellar 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.
* 1 2 3 4 5 6 7 8 9 10 11 12 13 14 15 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.
* 1 2 3 4 5 6 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.
* 1 2 GKK-A144 is a stellar association in Large Magellanic Cloud.
* ↑ BSDL 2242 is a star cluster in Large Magellanic Cloud.
* ↑ IC 4996 is an open cluster in Cygnus OB1.
* ↑ Vela R2 is a OB association in Vela Molecular Ridge.

## Black holes

Black holes are the end point of the 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 10000 M$_☉$ .
* Supermassive black holes are in the range of millions or billions M$_☉$.