List of most massive stars

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

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 determining the parameters needed to calculate the star's mass.

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 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,^[1] 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.^[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 infuses the adjacent volume of space 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.

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.^[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, on rare occasions, collide and merge when certain unusual circumstances hold that make a collision possible.^[3]

Eddington mass limit

Main article: Eddington luminosity

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.^[4]

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 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	Location	Mass (M☉)	Approx. dist. (ly)	Spectral type	Appt. vis. mag.	Eff. temp. (K)	Mass est. method	Link	Ref.
BAT99-98	Tarantula Nebula	226	165,000	WN6	13.37	45,000	spectroscopy	SIMBAD	[5][6]
R136a1	Tarantula Nebula	196+34 −27	163,000	WN5h	12.23	46,000	evolution	SIMBAD	[7][8]
Melnick 42	Tarantula Nebula	189	163,000	O2If*	12.78	47,300	spectroscopy	SIMBAD	[9][6]
VFTS 1022	Tarantula Nebula	178	164,000	O3.5If*/WN7	13.47	42,200	spectroscopy	SIMBAD	[9][6]
Westerhout 51-57	Westerhout 51	160	20,000	O4V	16.66 J band	42,700	evolution		[10]
R136a3	Tarantula Nebula	155	163,000	WN5h	12.97	50,000	evolution	SIMBAD	[7][8]
VFTS 682	Tarantula Nebula	153	164,000	WN5h	16.08	52,200	spectroscopy	SIMBAD	[11][6]
HD 15558 A	IC 1805	≥152±51	24,400	O5.5III(f)	7.87 combined	39,500	binary	SIMBAD	[12][13]
R136a2	Tarantula Nebula	151	163,000	WN5h	12.34	50,000	evolution	SIMBAD	[7][8]
Westerhout 51-3	Westerhout 51	148+105 −82	20,000	O3-8V	17.79 J band	39,800	evolution	SIMBAD	[10]
Melnick 34 A	Tarantula Nebula	147±22	163,000	WN5h	13.09 combined	53,000	binary	SIMBAD	[14][6]
VFTS 482	Tarantula Nebula	145	164,000	O3If*/WN6-A	12.95	42,200	spectroscopy	SIMBAD	[9][6]
R136c	Tarantula Nebula	142	163,000	WN5h	13.43	51,000	evolution	SIMBAD	[15][6]
VFTS 1021	Tarantula Nebula	141	164,000	O4 If+	13.35	39,800	spectroscopy	SIMBAD	[9][6]
LH 10-3209 A	NGC 1763	140	160,000	O3III(f*)	11.859 combined	42,500	spectroscopy	SIMBAD	[16][17][e]
Melnick 34 B	Tarantula Nebula	136±20	163,000	WN5h	13.09 combined	53,000	binary	SIMBAD	[14][6]
Westerhout 51d	Westerhout 51	135	20,000		15.11 J band	42,700	evolution		[10]
VFTS 545	Tarantula Nebula	133	164,000	O2If*/WN5	13.32	47,300	spectroscopy	SIMBAD	[9][6]
HD 97950 B	WR 43b in HD 97950	132	24,800	WN6h	11.33	42,000	spectroscopy	SIMBAD	[18][19]
HD 269810	NGC 2029	130	163,000	O2III(f*)	12.22	52,500	spectroscopy	SIMBAD	[20][21]
R136a7	Tarantula Nebula	127	163,000	O3III(f*)	13.97	54,000	evolution	SIMBAD	[22][6]
WR 42e	HD 97950	123	25,000	O3If*/WN6	14.53	43,000	Ejection	SIMBAD	[23][f]
VFTS 506	Tarantula Nebula	122	164,000	ON2V((n))((f*))	13.31	47,300	spectroscopy	SIMBAD	[11][6]
HD 97950 A1a	WR 43a A in HD 97950	120	24,800	WN6h	11.18 combined	42,000	binary	SIMBAD	[18][19]
LSS 4067	HM 1	120	11,000	O4.5Ifpe	11.44	40,000	evolution	SIMBAD	[24][25]
WR 93	Pismis 24	120	5,900	WC7	10.68	71,000	evolution	SIMBAD	[24][13]
Sk -69° 212	NGC 2044	119	160,000	O6If	12.416	45,400	evolution	SIMBAD	[26][17]
Sk -69° 249 A	NGC 2074	119	160,000	O7If	12.02 combined	38,900	evolution	SIMBAD	[26][27]
ST5-31	NGC 2074	119	160,000	O2-3(n)fp	12.273	50,700	evolution	SIMBAD	[26][28]
R136a5	Tarantula Nebula	116	157,000	O2I(n)f*	13.71	48,000	evolution	SIMBAD	[22][6]
MSP 183	Westerlund 2	115	20,000	O3V(f)	13.878	46,300	spectroscopy	SIMBAD	[29][30]
WR 24	Collinder 228	114	14,000	WN6ha-w	6.48	50,100	evolution	SIMBAD	[31][32]
HD 97950 C1	WR 43c A in HD 97950	113	24,800	WN6h	11.89 combined	44,000	spectroscopy	SIMBAD	[18][19][e]
Arches-F9	WR 102ae in Arches Cluster	111.3	25,000	WN8-9h	16.1 J band	36,600	spectroscopy	SIMBAD	[33][34]
Cygnus OB2 #12 A	Cygnus OB2	110	5,200	B3–4 Ia+	11.702 combined	13,700	spectroscopy	SIMBAD	[35][36][e]
HD 93129 Aa	Trumpler 14	110	7,500	O2If	6.9 combined	42,500	trinary	SIMBAD	[37][13]
HSH95-36	Tarantula Nebula	110	163,000	O2 If*	14.41	49,500	evolution	SIMBAD	[22][6]
R146	Tarantula Nebula	109	164,000	WN4	13.11	63,000	spectroscopy	SIMBAD	[5][6]
R136a4	Tarantula Nebula	108	157,000	O3 V((f*))(n)	13.41	50,000	evolution	SIMBAD	[22][6]
VFTS 621	Tarantula Nebula	107	164,000	O2V((f*))z	15.39	54,000	spectroscopy	SIMBAD	[9][6]
R136a6	Tarantula Nebula	105	157,000	O2I(n)f*p	13.35	52,000	evolution	SIMBAD	[22][6]
Westerhout 49-3	Westerhout 49	105	36,200	O3-O7V	16.689 J band	40,700	evolution	SIMBAD	[38][39]
WR 21a A	Runaway star from Westerlund 2	103.6	26,100	O3/WN5ha	12.661 combined	45,000	binary	SIMBAD	[40][21]
R99	N44	103	164,000	Ofpe/WN9	11.52	28,000	spectroscopy	SIMBAD	[5][13]
Arches-F6	WR 102ah in Arches Cluster	101	25,000	WN8-9h	15.75 J band	33,900	spectroscopy	SIMBAD	[33][34]
Sk -65° 47	NGC 1923	101	160,000	O4If	12.466	47,800	evolution	SIMBAD	[26][17]
Arches-F1	WR 102ad in Arches Cluster	100.9	25,000	WN8-9h	16.3 J band	33,200	spectroscopy	SIMBAD	[33][34]
HD 37836	Large Magellanic Cloud	100	163,000	B0Iae	10.55	28,200		SIMBAD	[41][42]
Peony Star	WR 102ka in Peony Nebula	100	26,000	Ofpe/WN9	12.978 J band	25,100	spectroscopy	SIMBAD	[43][39]
VFTS 457	Tarantula Nebula	100	164,000	O3.5If*/WN7	13.74	39,800	spectroscopy	SIMBAD	[9][6]
η Carinae A	Trumpler 16	100	7,500	LBV	4.3 combined	9,400–35,200	spectroscopy	SIMBAD	[44][45]
Mercer 30-1 A	WR 46-3 A in Mercer 30	99	40,000		10.33 J band	32,200	evolution	SIMBAD	[46][g][e]
Sk -68° 137	Tarantula Nebula	99	160,000		13.346	50,000	spectroscopy	SIMBAD	[16][17]
WR 25 A	Trumpler 16	98	6,500	O2.5If*	8.8 combined	50,100	evolution	SIMBAD	[31][13][e]
BI 253	runaway star from Tarantula Nebula	97.6	164,000	O2V	13.76	54,000	spectroscopy	SIMBAD	[15][47]
R136a8	Tarantula Nebula	96	157,000	O2–3V[48]	14.42	49,500	evolution	SIMBAD	[22][48]
HD 38282 B	Tarantula Nebula	95	163,000		11.11 combined	47,000	binary	SIMBAD	[49][21]
HM 1-6	HM 1	95	11,000		11.64	44,700	evolution	SIMBAD	[24][50]
NGC 3603-42	HD 97950	95	25,000		12.86	50,000	spectroscopy	SIMBAD	[16][19]
R139 A	Tarantula Nebula	95	163,000		11.94 combined	35,000	binary	SIMBAD	[5][6]
BAT99-6	NGC 1747	94	165,000		11.95	56,000	spectroscopy	SIMBAD	[5][17]
Sk -66° 172	N64	94	160,000		13.1	46,300	spectroscopy	SIMBAD	[16][17][h]
ST2-22	NGC 2044	94	160,000		14.3	51,300	evolution	SIMBAD	[26][51]
VFTS 259	Tarantula Nebula	94	164,000		13.65	37,600	spectroscopy	SIMBAD	[9][6]
VFTS 562	Tarantula Nebula	94	164,000		13.66	42,200	spectroscopy	SIMBAD	[9][6]
VFTS 512	Tarantula Nebula	93	164,000		14.28	47,300	spectroscopy	SIMBAD	[9][6]
HD 97950 A1b	WR 43a B in HD 97950	92	24,800	WN6h[52]	11.18 combined	40,000	binary	SIMBAD	[18][19]
R136b	Tarantula Nebula	92	163,000		13.24	35,500	evolution	SIMBAD	[22][6]
VFTS 16	Tarantula Nebula	91.6	164,000		13.55	50,600	spectroscopy	SIMBAD	[15][6]
HD 97950 A3	HD 97950	91	24,800		12.95	50,000	spectroscopy	SIMBAD	[16][19]
NGC 346-W1	NGC 346	91	200,000		12.57	43,400	evolution	SIMBAD	[26][53]
Westerhout 49-2	Westerhout 49	90–240, 250±120	36,200		18.246 J band	35,500	spectroscopy	SIMBAD	[38][39]
R127	NGC 2055	90	160,000		10.15	10,000–27,000	evolution	SIMBAD	[54][21]
VFTS 333	Tarantula Nebula	90	164,000		12.49	37,600	spectroscopy	SIMBAD	[9][6]
VFTS 267	Tarantula Nebula	89	164,000		13.49	44,700	spectroscopy	SIMBAD	[9][6]
VFTS 64	Tarantula Nebula	88	164,000		14.621	39,800	spectroscopy	SIMBAD	[9][17]
BAT99-80 A	NGC 2044	87	165,000		13 combined	45,000	spectroscopy	SIMBAD	[26][51]
R140b	Tarantula Nebula	87	165,000		12.66	47,000	spectroscopy	SIMBAD	[5][6]
VFTS 542	Tarantula Nebula	87	164,000		13.47	44,700	spectroscopy	SIMBAD	[9][6]
VFTS 599	Tarantula Nebula	87	164,000		13.8	44,700	spectroscopy	SIMBAD	[9][6]
WR 89	HM 1	87	11,000		11.02	39,800	evolution	SIMBAD	[31][21]
Arches-F7	WR 102aj in Arches Cluster	86.3	25,000		15.74 J band	32,900	spectroscopy	SIMBAD	[33][34]
Sk -69° 104	NGC 1910	86	160,000		12.1	39,900	evolution	SIMBAD	[26][17]
VFTS 1017	Tarantula Nebula	86	164,000		14.5	50,100	spectroscopy	SIMBAD	[9][6]
LH 10-3061	NGC 1763	85	160,000		13.491	52,000	spectroscopy	SIMBAD	[16][17]
Sk 80	NGC 346	85	200,000		12.31	38,900	evolution	SIMBAD	[26][55]
VFTS 603	Tarantula Nebula	85	164,000		13.99	42,200	spectroscopy	SIMBAD	[9][6]
Sk -70° 91	BSDL 1830	84.09	165,000		12.78	48,900	evolution	SIMBAD	[56][17][i]
R147	Tarantula Nebula	84	164,000		12.993	47,300	spectroscopy	SIMBAD	[9][57]
HD 93250 A	Trumpler 16	83.3	7,500		7.5 combined	46,000	evolution	SIMBAD	[58][13][e]
Melnick 33Na A	Tarantula Nebula	83	163,000		13.79 combined	50,000	evolution	SIMBAD	[59][60]
WR 20a A	Westerlund 2	82.7	20,000		13.28 combined	43,000	binary	SIMBAD	[61]
TIC 276934932 A	NGC 2048	82	160,000		14.05 combined	45,000	spectroscopy	SIMBAD	[16][17]
WR 20a B	Westerlund 2	81.9	20,000		13.28 combined	43,000	binary	SIMBAD	[61]
Trumpler 27-27	Trumpler 27	81	3,900		13.31	37,000	evolution	SIMBAD	[24][21]
BAT99-96	Tarantula Nebula	80	165,000		13.76	42,000	spectroscopy	SIMBAD	[5][6]
HD 15570	IC 1805	80	7,500		8.11	46,000	spectroscopy	SIMBAD	[12][13]
HD 38282 A	Tarantula Nebula	80	163,000		11.11 combined	47,000	binary	SIMBAD	[49][21]
HSH95-46	Tarantula Nebula	80	163,000		14.56	47,500	evolution	SIMBAD	[22][6]
Arches-F15	Arches Cluster	79.7	25,000		16.12 J band	35,600	spectroscopy	SIMBAD	[33][34]
BI 237	BSDL 2527	79.66	165,000		13.83	51,300	spectroscopy	SIMBAD	[56][17][j]
VFTS 94	Tarantula Nebula	79	164,000		14.161	42,200	spectroscopy	SIMBAD	[9][17]
VFTS 151	Tarantula Nebula	79	164,000		14.13	42,200	spectroscopy	SIMBAD	[9][6]
LH 41-32	NGC 1910	78	160,000		13.086	48,200	evolution	SIMBAD	[26][17]
Pismis 24-17	Pismis 24	78	5,900		11.84	42,700	spectroscopy	SIMBAD	[62][50]
VFTS 404	Tarantula Nebula	78	164,000		14.14	44,700	spectroscopy	SIMBAD	[9][6]
Westerhout 51-2	Westerhout 51	77+26 −22	20,000		13.68 J band	42,700	evolution	SIMBAD	[10]
BAT99-68	BSDL 2505	76	165,000		14.13	45,000	spectroscopy	SIMBAD	[5][17][k]
HD 93632	Collinder 228	76	10,000		8.23	45,400	evolution	SIMBAD	[24][13]
NGC 346-W3	NGC 346	76	200,000		12.8	52,500	evolution	SIMBAD	[26][53]
VFTS 169	Tarantula Nebula	76	164,000		14.437	47,300	spectroscopy	SIMBAD	[9][17]
VFTS 440	Tarantula Nebula	76	164,000		12.046	39,800	spectroscopy	SIMBAD	[9][17]
AB1	DEM S10	75	197,000		15.238	79,000	spectroscopy	SIMBAD	[63][53][l]
WR 22 A	Bochum 10	75	8,300		6.42 combined	44,700	evolution	SIMBAD	[31][13][m]
Pismis 24-1NE	Pismis 24	74	6,500		11	42,500	binary	SIMBAD	[62][64]
VFTS 608	Tarantula Nebula	74	164,000		14.22	42,200	spectroscopy	SIMBAD	[9][6]
HSH95-31	Tarantula Nebula	73	163,000		14.12	47,500	evolution	SIMBAD	[22][6]
Mercer 30-3	Mercer 30	73	40,000		12.62 J band	39,300	evolution	SIMBAD	[46][g]
Mercer 30-11	Mercer 30	73	40,000		12.33 J band	36,800	evolution	SIMBAD	[46][g]
VFTS 566	Tarantula Nebula	73	164,000		14.05	44,700	spectroscopy	SIMBAD	[9][6]
LH 64-16	NGC 2001	72	160,000		13.666	50,900	evolution	SIMBAD	[26][28]
NGC 2044-W35	NGC 2044	72	160,000		14.1	48,200	evolution	SIMBAD	[26][17]
VFTS 216	Tarantula Nebula	72	164,000		14.389	44,700	spectroscopy	SIMBAD	[9][17]
ST2-1	NGC 2044	71	160,000		14.3	44,100	evolution	SIMBAD	[26][51]
VFTS 3	Tarantula Nebula	71	164,000		11.56	21,000	spectroscopy	SIMBAD	[65][6]
Arches-F12	WR 102af in Arches Cluster	70	25,000		16.4 J band	36,900	spectroscopy	SIMBAD	[33][34]
HD 15629	IC 1805	70	7,500		8.42	45,900	spectroscopy	SIMBAD	[12][13]
HD 37974	N135	70	163,000		10.99	22,500	spectroscopy	SIMBAD	[66][21][n]
HD 93129 Ab	Trumpler 14	70	7,500		7.31 combined	44,000	trinary	SIMBAD	[37][67]
M33 X-7 B	Triangulum Galaxy	70	2,700,000		18.7	35,000	binary	SIMBAD	[68][69]
Sk -69° 194 A	NGC 2033	70	160,000		12.131 combined	45,000	evolution	SIMBAD	[26][57][e]
VFTS 125	Tarantula Nebula	69.6	164,000		16.6	55,200	spectroscopy	SIMBAD	[15][51]
HD 46150	NGC 2244	69	5,200		6.73	44,000	spectroscopy	SIMBAD	[16][13]
HD 229059	Berkeley 87	69	3,000		8.7	26,300	evolution	SIMBAD	[24][13]
ST2-3	NGC 2044 of LMC	69	160,000		14.264	44,900	evolution	SIMBAD	[26][17]
ST2-32	NGC 2044	69	160,000		13.903	45,400	evolution	SIMBAD	[26][17]
W28-23	NGC 2033	69	160,000		13.702	51,300	evolution	SIMBAD	[26][28]
HD 93403 A	Trumpler 16	68.5	10,400		8.27 combined	39,300	binary	SIMBAD	[70][21]
HD 93130	Collinder 228	68	10,000	O7II(f)[71]	8.04	39,900	evolution	SIMBAD	[24][13]
HM 1-8	HM 1	68	11,000		12.52	46,100	evolution	SIMBAD	[24][50]
HSH95-47	Tarantula Nebula	68	163,000		14.72	43,500	evolution	SIMBAD	[22][6]
HSH95-48	Tarantula Nebula	68	163,000		14.75	46,500	evolution	SIMBAD	[22][48]
Westerhout 51-61	Westerhout 51	68	20,000		18.16 J band	38,000	evolution	SIMBAD	[10][39]
BAT99-93	Tarantula Nebula	67	165,000		13.446	45,000	spectroscopy	SIMBAD	[5][17]
Sk -69° 200	NGC 2033	67	160,000		11.18	26,300	evolution	SIMBAD	[26][17]
Arches-F18	Arches Cluster	66.9	25,000		16.7 J band	36,900	spectroscopy	SIMBAD	[33][34]
Arches-F4	WR 102al in Arches Cluster	66.4	25,000		15.63 J band	36,800	spectroscopy	SIMBAD	[33][34]
BAT99-59 A	NGC 2020	66	165,000		13.186 combined	71,000	spectroscopy	SIMBAD	[5][17][e]
BAT99-104	Tarantula Nebula	66	165,000		12.5	63,000	spectroscopy	SIMBAD	[5][17]
HD 5980 B	NGC 346	66	200,000		11.31 combined	45,000	trinary	SIMBAD	[72][67]
HD 190429 A	near Barnard 146	66	7,800		6.63 combined	46,000	binary	SIMBAD	[73][13]
LH 31-1003	NGC 1858	66	160,000		13.186	41,900	evolution	SIMBAD	[26][17]
LH 114-7	N70	66	160,000		13.66	50,000	spectroscopy	SIMBAD	[16][17][o]
Pismis 24-1SW	Pismis 24	66	6,500		11.1	40,000	binary	SIMBAD	[62][64]
BAT99-126	NGC 2081	65	165,000		13.166	71,000	spectroscopy	SIMBAD	[5][17]
HSH95-40	Tarantula Nebula	65	163,000		14.56	47,500	evolution	SIMBAD	[22][6]
HSH95-58	Tarantula Nebula	65	163,000		14.8	47,500	evolution	SIMBAD	[22][6]
HSH95-89	Tarantula Nebula	65	163,000		14.76	44,000	spectroscopy	SIMBAD	[48]
VFTS 63	Tarantula Nebula	65	164,000		14.4	42,200	spectroscopy	SIMBAD	[9][51]
VFTS 145	Tarantula Nebula	65	164,000		14.3	39,800	spectroscopy	SIMBAD	[9][6]
VFTS 518	Tarantula Nebula	65	164,000		15.11	44,700	spectroscopy	SIMBAD	[9][6]
Westerhout 49-8	Westerhout 49	65	36,200		15.617 J band	40,700	evolution	SIMBAD	[38][39]
BD+43° 3654	Runaway star from Cygnus OB2	64.6	5,400		10.06	40,400	evolution	SIMBAD	[74][67]
BAT99-129 A	DEM L294	64	165,000		14.701 combined	79,000	spectroscopy	SIMBAD	[5][17][p][e]
HSH95-50	Tarantula Nebula	64	163,000		14.65	47,000	evolution	SIMBAD	[22][6]
Sk -69° 25	NGC 1748	64	160,000		11.886	43,600	evolution	SIMBAD	[26][17]
Trumpler 27-23	Trumpler 27	64	3,900		10.09	27,500	evolution	SIMBAD	[24][21]
Westerhout 49-5	Westerhout 49	64	36,200		15.623 J band	42,700	evolution	SIMBAD	[38][39]
HD 46223	NGC 2244	63	5,200		7.28	46,000	spectroscopy	SIMBAD	[16][13]
HD 64568	NGC 2467	63	16,000		9.39	54,000	spectroscopy	SIMBAD	[16][21]
HD 303308	Trumpler 16	63	9,200		8.17	51,300	evolution	SIMBAD	[24][21]
HR 6187 A	NGC 6193	63	4,300		5.54 combined	46,500	Septenary	SIMBAD	[75][13]
LH 10-3058	NGC 1763	63	160,000		14.089	54,000	spectroscopy	SIMBAD	[16][17]
ST5-71	NGC 2074	63	160,000		13.266	45,400	evolution	SIMBAD	[26][17]
AB9	DEM S80	62	197,000		15.431	100,000	spectroscopy	SIMBAD	[63][53][q]
Brey 32 B	NGC 1966	62	165,000		12.32 combined	43,600	evolution	SIMBAD	[26][21]
HD 93160	Trumpler 14	62	8,000		7.6	42,700	evolution	SIMBAD	[24][13]
HSH95-35	Tarantula Nebula	62	163,000		14.43	47,500	evolution	SIMBAD	[22][6]
LH 41-1017	NGC 1910	62	160,000		12.266	42,700	evolution	SIMBAD	[26][17]
Mercer 30-6a A	WR 46-4 A in Mercer 30	62	40,000		10.39 J band	29,900	evolution	SIMBAD	[46][g][e]
ST4-18	NGC 2081	62	160,000		13.639	44,800	evolution	SIMBAD	[26][17]
VFTS 664	Tarantula Nebula	62	164,000		13.937	39,900	spectroscopy	SIMBAD	[9][17]
HD 229196	Cygnus OB9	61.6	5,000		8.59	40,900	evolution	SIMBAD	[74][50]
AB8 B	NGC 602	61	197,000	O4V	12.83 combined	45,000	binary	SIMBAD	[72][76]
BAT99-79 A	NGC 2044	61	165,000		13.486 combined	42,000	spectroscopy	SIMBAD	[5][17][e]
HD 5980 A	NGC 346	61	200,000		11.31 combined	21,000–53,000	trinary	SIMBAD	[72][67]
LH 41-18	NGC 1910	61	160,000		12.586	38,500	evolution	SIMBAD	[26][17]
Mercer 30-9 A	Mercer 30	61	40,000		12.25 J band	34,500	evolution	SIMBAD	[46][g][e]
ST5-25	NGC 2074	61	160,000		13.551	48,600	evolution	SIMBAD	[26][28]
VFTS 422	Tarantula Nebula	61	164,000		15.14	39,800	spectroscopy	SIMBAD	[9][6]
WR 102hb	Quintuplet cluster	61	26,000		13.9 J band	25,100	evolution	SIMBAD	[77][78]
Sk -67° 166	GKK-A144	60.68	160,000		12.22	41,800	spectroscopy	SIMBAD	[56][17][r]
Sk -67° 167	GKK-A144	60.68	160,000		12.586	41,800	spectroscopy	SIMBAD	[56][17][r]
Sk -71° 46	BSDL 2242	60.68	160,000		13.241	41,800	spectroscopy	SIMBAD	[56][17][s]
Brey 10	NGC 1770	60	165,000		12.69	117,000	evolution	SIMBAD	[26][21]
Brey 94 A	NGC 2081	60	165,000		12.996 combined	83,000	evolution	SIMBAD	[26][17][e]
Brey 95a A	NGC 2081	60	165,000		12.2 combined	83,000	evolution	SIMBAD	[26][79][e]
HSH95-55	Tarantula Nebula	60	163,000		14.74	47,500	evolution	SIMBAD	[22][6]
Mercer 30-7 A	WR 46-5 A in Mercer 30	60	40,000		11.516 J band	41,400	evolution	SIMBAD	[46][g][e]
R134	Tarantula Nebula	60	164,000		12.75	39,800	spectroscopy	SIMBAD	[9][6]
R142	Tarantula Nebula	60	164,000		11.82	18,000	spectroscopy	SIMBAD	[65][6]
R143	Tarantula Nebula	60	160,000		12.014	18,000–36,000	evolution	SIMBAD	[54][17]
Sk -69° 142a	NGC 1983	60	160,000		11.093	34,000	evolution	SIMBAD	[54][57]
Sk -69° 259	NGC 2081	60	160,000		11.93	23,000	evolution	SIMBAD	[26][21]
Var 83	Triangulum Galaxy	60	3,000,000		16.027	18,000–37,000	evolution	SIMBAD	[80][81]
VFTS 430	Tarantula Nebula	60	164,000		15.11	24,500	spectroscopy	SIMBAD	[65][6]

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	Ref.
λ Cephei	Runaway star from Cepheus OB3	51.4	3,100	5.05	36,000	spectroscopy	SIMBAD	[73][13]
τ Canis Majoris Aa	NGC 2362	50	5,120	4.89	32,000	evolution	SIMBAD	[82][13]
θ Muscae Ab	Centaurus OB1	44	7,400	5.53 combined	33,000	evolution	SIMBAD	[83][13]
ε Orionis	Alnilam in Orion OB1 of Orion complex	40	2,000	1.69	27,500	evolution	SIMBAD	[84][13]
θ2 Orionis A	Orion OB1 of Orion complex	39	1,500	5.02	34,900	evolution	SIMBAD	[85][86]
α Camelopardalis	Runaway star from NGC 1502	37.6	6,000	4.29	29,000	evolution	SIMBAD	[87][13]
P Cygni	IC 4996 of Cygnus OB1	37	5,100	4.82	18,700	spectroscopy	SIMBAD	[88][13][t]
ζ1 Scorpii	NGC 6231 of Scorpius OB1	36	8,210	4.705	17,200	spectroscopy	SIMBAD	[35][89]
ζ Orionis Aa	Alnitak in Orion OB1 of Orion complex	33	1,260	2.08	29,500	evolution	SIMBAD	[90]
θ1 Orionis C1	Trapezium Cluster of Orion complex	33	1,340	5.13 combined	39,000	evolution	SIMBAD	[91][13]
κ Cassiopeiae	Cassiopeia OB14	33	4,000	4.16	23,500	evolution	SIMBAD	[92][13]
μ Normae	NGC 6169	33	3,260	4.91	28,000	spectroscopy	SIMBAD	[93][13]
η Carinae B	Trumpler 16 of Carina Nebula	30	7,500	4.3 combined	37,200	binary	SIMBAD	[94][45]
γ2 Velorum B	Vela OB2	28.5	1,230	1.83 combined	35,000	evolution	SIMBAD	[95][13]
Meissa A	In Collinder 69 of Orion complex	27.9	1,100	3.54	37,700	spectroscopy	SIMBAD	[93][96]
ξ Persei	Menkib in California Nebula of Perseus OB2	26.1	1,200	4.04	35,000	evolution	SIMBAD	[87][13]
ζ Puppis	Naos in Vela R2 of Vela Molecular Ridge	25.3±5.3	1,080	2.25	40,000	empirical	SIMBAD	[97][13][u]
WR 79a	NGC 6231 of Scorpius OB1	24.4	5,600	5.77	35,000	spectroscopy	SIMBAD	[93][13]
Mintaka Aa1	In Orion OB1 of Orion complex	24	1,200	2.5 combined	29,500	evolution	SIMBAD	[98][99]
ι Orionis Aa1	Hatysa in NGC 1980 of Orion complex	23.1	1,340	2.77 combined	32,500	evolution	SIMBAD	[100][101]
κ Crucis	Jewel Box Cluster of Centaurus OB1	23	7,500	5.98	16,300	evolution	SIMBAD	[102][67]
WR 78	NGC 6231 of Scorpius OB1	22	4,100	6.48	50,100	spectroscopy	SIMBAD	[31][32]
ο2 Canis Majoris	Field star	21.4	2,800	3.043	15,500	evolution	SIMBAD	[93][13]
Rigel A	In Orion OB1 of Orion complex	21	860	0.13	12,100	evolution	SIMBAD	[103][13]
η Canis Majoris	Aludra in Collinder 121	21	2,000	2.45	15,000	evolution	SIMBAD	[92][13]
ζ Ophiuchi	Upper Scorpius subgroup of Scorpius OB2	20.2	370	2.569	34,000	evolution	SIMBAD	[87][13]
υ Orionis	Orion OB1 of Orion complex	20	2,900	4.618	33,400	evolution	SIMBAD	[104][105]
σ Orionis Aa	Orion OB1 of Orion complex	18	1,260	4.07 combined	35,000	spectroscopy	SIMBAD	[106][107]
μ Columbae	Runaway star from Trapezium Cluster	16	1,300	5.18	33,000	spectroscopy	SIMBAD	[108][13]
Saiph	In Orion OB1 of Orion complex	15.5	650	2.09	26,500	evolution	SIMBAD	[109][13]
σ Cygni	Cygnus OB4	15	3,260	4.233	10,800	evolution	SIMBAD	[110][111]
θ Carinae A	IC 2602 of Scorpius OB2	14.9	460	2.76 combined	31,000	evolution	SIMBAD	[93][112]
θ2 Orionis B	Orion OB1 of Orion complex	14.8	1,500	6.38	29,300	spectroscopy	SIMBAD	[113]
ζ Persei	Perseus OB2	14.5	750	2.86	20,800	evolution	SIMBAD	[109][13]
σ Orionis B	Orion OB1 of Orion complex	14	1,260	4.07 combined	31,000	spectroscopy	SIMBAD	[106][107]
β Canis Majoris	Mirzam in Local Bubble of Scorpius OB2	13.5	490	1.985	23,200	evolution	SIMBAD	[114][115]
ε Persei A	α Persei Cluster	13.5	640	2.88 combined	26,500	evolution	SIMBAD	[116][117]
ι Orionis Aa2	NGC 1980 of Orion complex	13.1	1,340	2.77 combined	27,000	evolution	SIMBAD	[100][101]
δ Scorpii A	Dschubba in Upper Scorpius subgroup of Scorpius OB2	13	440	2.307 combined	27,400	evolution	SIMBAD	[118][119]
σ Orionis Ab	Orion OB1 of Orion complex	13	1,260	4.07 combined	29,000	spectroscopy	SIMBAD	[106][107]
θ Muscae Aa	WR 48 in Centaurus OB1	11.5	7,400	5.53 combined	83,000	spectroscopy	SIMBAD	[120][13]
γ2 Velorum A	WR 11 in Vela OB2	9	1,230	1.83 combined	57,000	spectroscopy	SIMBAD	[95][13]
ρ Ophiuchi A	ρ Ophiuchi cloud complex of Scorpius OB2	8.7	360	4.63 combined	22,000	evolution	SIMBAD	[93][13]
Bellatrix	In Bellatrix Cluster of Orion complex	7.7	250	1.64	21,800	evolution	SIMBAD	[121][13]
Antares B	Loop I Bubble of Scorpius OB2	7.2	550	5.5	18,500	evolution	SIMBAD	[122][96]
λ Tauri A	Pisces-Eridanus stellar stream	7.18	480	3.47 combined	18,700	evolution	SIMBAD	[123][124]
δ Persei	α Persei Cluster	7	520	3.01	14,900	evolution	SIMBAD	[93][112]
ψ Persei	α Persei Cluster	6.2	580	4.31	16,000	evolution	SIMBAD	[93][13]
α Pavonis Aa	Peacock in Tucana-Horologium association	5.91	180	1.94	17,700	evolution	SIMBAD	[125][101]
Alcyone	In Pleiades	5.9	440	2.87 combined	12,300	evolution	SIMBAD	[126][13]
γ Canis Majoris	Muliphein in Collinder 121	5.6	440	4.1	13,600	evolution	SIMBAD	[93][127]
ο Velorum	IC 2391 of Scorpius OB2	5.5	490	3.6	16,200	evolution	SIMBAD	[128][112]
ο Aquarii	Pisces-Eridanus stellar stream	4.2	440	4.71	13,500	evolution	SIMBAD	[129][130]
ν Fornacis	Pisces-Eridanus stellar stream	3.65	370	4.69	13,400	evolution	SIMBAD	[131][13]
φ Eridani	Tucana-Horologium association	3.55	150	3.55	13,700	evolution	SIMBAD	[125][132]
η Chamaeleontis	η Chamaeleontis moving group of Scorpius OB2	3.2	310	5.453	12,500	evolution	SIMBAD	[133][67]
ε Chamaeleontis	ε Chamaeleontis moving group of Scorpius OB2	2.87	360	4.91	10,900	evolution	SIMBAD	[134][112]
τ1 Aquarii	Pisces-Eridanus stellar stream	2.68	320	5.66	10,600	evolution	SIMBAD	[135][136]
ε Hydri	Tucana-Horologium association	2.64	150	4.12	11,000	evolution	SIMBAD	[135][137]
β1 Tucanae	Tucana-Horologium association	2.5	140	4.37	10,600	evolution	SIMBAD	[93][96]
Sun	Solar System	1	0.0000158	−26.744	5,772	standard	IAU	[138][139][140]

1. For some methods, for any one temperature or brightness, different chemical composition indicates a different estimate for stellar 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. 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. 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. GKK-A144 is a stellar association in Large Magellanic Cloud.
19. BSDL 2242 is a star cluster in Large Magellanic Cloud.
20. IC 4996 is an open cluster in Cygnus OB1.
21. Vela R2 is a OB association in Vela Molecular Ridge.

Black holes

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

Black holes are the end point of the evolution of massive stars.^[A] 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_☉.

See also

• Hypergiant
• 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 stars
• List of most luminous stars
• List of most massive black holes
• List of most massive neutron stars
• List of most massive star clusters
• Lists of stars
• Luminous blue variable
• Supergiant
• Supernova impostor
• Wolf–Rayet star

Footnotes

1. A very few low / no metallicity stars (populations II and III) between 140–250 M_☉ end their lives by a type II-P supernova explosion, which is powerful enough to blow (almost) all matter away from the vicinity of the star, so that not enough material remains to create either a black hole, or a neutron star, or a white dwarf: There is no central remnant; all that remains is an expanding shell of shocked gas from the SN explosion colliding with previously quiescent material ejected before the core collapse explosion.

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.
• "How heavy can a star get?". 3towers. Archived from the original on 2007-10-28.
• "Hubble Unveils Monster Stars". NASA. March 2016.