List of most massive stars

 ( Massive ) 

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

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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 ' temperatures, metallicity, 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.

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Complications with distance and obscuring clouds Since massive stars are rare, 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 ; 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 120-solar-mass range, so any mass estimate above this range is suspect.

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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 velocity 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.

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Relevance of stellar evolution Some stars may once have been more massive than they are today. Many large stars have likely suffered significant mass loss (perhaps as much as several tens of solar masses). The lost mass is expected to have been expelled by : 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 – 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).

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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 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 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.

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Accretion limits Astronomers have long hypothesized that as a protostar grows to a size beyond 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 they would challenge current theories of stellar evolution.

Studying the Arches Cluster, which is currently the densest known cluster of stars in Milky Way, astronomers have confirmed that no stars in that cluster exceed about

Rare ultramassive stars that exceed this limit – for example in the R136 star cluster – might be explained by an exceptional event hypothesized to have occurred: some of the pairs of massive binary star in young, unstable multiple-star systems must, on rare occasions, collide and merge when certain unusual circumstances hold that make a collision possible.

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Eddington mass limit Arthur 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 .

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.

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List of the most massive known stars

+ Legend

The following two lists show a few of the known stars, including the stars in , , 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  or larger; the majority of which are shown. The second list includes some notable stars which are below 60  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  or greater
R136a1			163,000	WN5h	12.23	46,000
BAT99-98		226	165,000	WN6	13.37	45,000
R136a2			163,000	WN5h	12.34	50,000
Melnick 42		189	163,000	O2If*	12.78	47,300
R136a3			163,000	WN5h	12.97	50,000
VFTS 1022		178	164,000	O3.5If*/WN7	13.47	42,200
Westerhout 51-57		160	20,000	O4V	16.66	42,700
VFTS 682		153	164,000	WN5h	16.08	52,200
HD 15558 A		≥	24,400	O5.5III(f)	7.87	39,500
Westerhout 51-3			20,000	O3-8V	17.79	39,800
Melnick 34 A			163,000	WN5h	13.09	53,000
R136c		142	163,000	WN5h	13.43	51,000
VFTS 1021		141	164,000	O4 If+	13.35	39,800
LH 10-3209 A		140	160,000	O3III(f*)	11.859	42,500
Melnick 34 B			163,000	WN5h	13.09	53,000
Westerhout 51d		135	20,000		15.11	42,700
VFTS 545		133	164,000	O2If*/WN5	13.32	47,300
HD 97950 B		132	24,800	WN6h	11.33	42,000
HD 269810		130	163,000	O2III(f*)	12.22	52,500
R136a7		127	163,000	O3III(f*)	13.97	54,000
WR 42e		123	25,000	O3If*/WN6	14.53	43,000
VFTS 506		122	164,000	ON2V((n))((f*))	13.31	47,300
HD 97950 A1a		120	24,800	WN6h	11.18	42,000
LSS 4067		120	11,000	O4.5Ifpe	11.44	40,000
WR 93		120	5,900	WC7	10.68	71,000
Sk -69° 212		119	160,000	O6If	12.416	45,400
Sk -69° 249 A		119	160,000	O7If	12.02	38,900
ST5-31		119	160,000	O2-3(n)fp	12.273	50,700
R136a5		116	157,000	O2I(n)f*	13.71	48,000
MSP 183		115	20,000	O3V(f)	13.878	46,300
WR 24		114	14,000	WN6ha-w	6.48	50,100
HD 97950 C1		113	24,800	WN6h	11.89	44,000			This is a binary system but the secondary is much less massive than the primary.
Arches Cluster-F9		111.3	25,000	WN8-9h	16.1	36,600
Cygnus OB2 #12 A		110	5,200	B3–4 Ia+	11.702	13,700
HD 93129 Aa		110	7,500	O2If	6.9	42,500
HSH95-36		110	163,000	O2 If*	14.41	49,500
R146		109	164,000	WN4	13.11	63,000
R136a4		108	157,000	O3 V((f*))(n)	13.41	50,000
VFTS 621		107	164,000	O2V((f*))z	15.39	54,000
R136a6		105	157,000	O2I(n)f*p	13.35	52,000
Melnick 39 A		≥	160,000	O2.5 If/WN6	13.0	44,000
Westerhout 49-3		105	36,200	O3-O7V	16.689	40,700
WR 21a A		103.6	26,100	O3/WN5ha	12.661	45,000
R99		103	164,000	Ofpe/WN9	11.52	28,000
Arches Cluster-F6		101	25,000	WN8-9h	15.75	33,900
Sk -65° 47		101	160,000	O4If	12.466	47,800
Arches Cluster-F1		100.9	25,000	WN8-9h	16.3	33,200
HD 37836	Large Magellanic Cloud	100	163,000	B0Iae	10.55	28,200		SIMBAD
Peony Star		100	26,000	Ofpe/WN9	12.978	25,100
VFTS 457		100	164,000	O3.5If*/WN7	13.74	39,800
Eta Carinae A		100	7,500	LBV	4.3	9,400–35,200
Mercer 30-1 A		99	40,000	O6-7.5If+	10.33	32,200			Mercer 30 is an open cluster in Dragonfish Nebula.
Sk -68° 137		99	160,000	OB	13.346	50,000
WR 25 A		98	6,500	O2.5If*	8.8	50,100
BI 253		97.6	164,000	O2V	13.76	54,000
R136a8		96	157,000	O2–3V	14.42	49,500
HD 38282 B		95	163,000	WN6/7h	11.11	47,000
HM 1-6		95	11,000	O5.5Ifc	11.64	44,700
NGC 3603-42		95	25,000	O3III	12.86	50,000
R139 A		95	163,000	O6.5Iafc	11.94	35,000
BAT99-6		94	165,000	O6-7n-nn+WN5-6-A	11.95	56,000
Sk -66° 172		94	160,000	O2III(f*)+OB	13.1	46,300			N64 is an emission nebula in Large Magellanic Cloud.
ST2-22		94	160,000	O3.5III(f+)	14.3	51,300
VFTS 259		94	164,000	O6Iaf	13.65	37,600
VFTS 562		94	164,000	O4III(f)	13.66	42,200
			24,800	WN6h	11.18	37,000
VFTS 512		93	164,000	O2V-III((f*))	14.28	47,300
R136b		92	163,000	WN9ha	13.24	35,500
VFTS 16		91.6	164,000	O2IIIf*	13.55	50,600
HD 97950 A3		91	24,800	O3III(f*)	12.95	50,000
NGC 346-W1		91	200,000	O4If+O5-6	12.57	43,400
Westerhout 49-2		90–240,	36,200	O2-3.5If*	18.246	35,500
R127		90	160,000	LBV	10.15	10,000–27,000
VFTS 333		90	164,000	O7/8II	12.49	37,600
VFTS 267		89	164,000	O3III-I(n)f*	13.49	44,700
VFTS 64		88	164,000	O7.5II(f)	14.621	39,800
BAT99-80 A		87	165,000	O4If+OB	13	45,000
R140b		87	165,000	WN6	12.66	47,000
VFTS 542		87	164,000	O2If*/WN5	13.47	44,700
VFTS 599		87	164,000	O3III(f*)	13.8	44,700
WR 89		87	11,000	WN8h	11.02	39,800
Arches Cluster-F7		86.3	25,000	WN8-9h	15.74	32,900
Sk -69° 104		86	160,000	O6Ib(f)	12.1	39,900
VFTS 1017		86	164,000		14.5	50,100
LH 10-3061		85	160,000	ON2III(f*)	13.491	52,000
Sk 80		85	200,000	O7Iaf+	12.31	38,900
VFTS 603		85	164,000	O4III(fc)	13.99	42,200
Sk -70° 91		84.09	165,000	O2III(f*)+OB	12.78	48,900			BSDL 1830 is a star cluster in Large Magellanic Cloud.
R147		84	164,000	WN5h	12.993	47,300
HD 93250 A		83.3	7,500	O4III(fc)	7.5	46,000
		83	163,000		13.79	50,000
WR 20a A		82.7	20,000	O3If*/WN6+O3If*/WN6	13.28	43,000
TIC 276934932 A		82	160,000	O3If+O6V	14.05	45,000
WR 20a B		81.9	20,000	O3If*/WN6+O3If*/WN6	13.28	43,000
Trumpler 27-27		81	3,900	O8III	13.31	37,000
BAT99-96		80	165,000	WN8	13.76	42,000
HD 15570		80	7,500	O4If	8.11	46,000
HD 38282 A		80	163,000	WN5/6h+WN6/7h	11.11	47,000
HSH95-46		80	163,000		14.56	47,500
Melnick 39 B		≥	160,000	O3 V-III	13.0	48,000
Arches Cluster-F15		79.7	25,000	O4-6If	16.12	35,600
BI 237		79.66	165,000	O2V(f*)	13.83	51,300			BSDL 2527 is a star cluster in Large Magellanic Cloud.
VFTS 94		79	164,000	O3.5Inf*p+sec?	14.161	42,200
VFTS 151		79	164,000	O6.5II(f)p	14.13	42,200
LH 41-32		78	160,000	O4III	13.086	48,200
Pismis 24-17		78	5,900	O3.5III(f*)	11.84	42,700
VFTS 404		78	164,000	O3.5V(n)((fc))	14.14	44,700
Westerhout 51-2			20,000	O3-5V	13.68	42,700
BAT99-68		76	165,000	O3If*/WN6	14.13	45,000			BSDL 2505 is a star cluster in Large Magellanic Cloud.
HD 93632		76	10,000	O5Ifvar	8.23	45,400
NGC 346-W3		76	200,000	O2III(f)	12.8	52,500
VFTS 169		76	164,000	O2.5V(n)((f*))	14.437	47,300
VFTS 440		76	164,000	O6-6.5II(f)	12.046	39,800
AB1		75	197,000	WN3+O4:	15.238	79,000			DEM S10 is a H II region in Small Magellanic Cloud.
WR 22 A		75	8,300	WN7h+O9III-V	6.42	44,700			Bochum 10 is an open cluster in Carina Nebula.
Pismis 24-1NE		74	6,500		11	42,500
VFTS 608		74	164,000	O4III(f)	14.22	42,200
HSH95-31		73	163,000		14.12	47,500
Mercer 30-3		73	40,000	O6If	12.62	39,300
Mercer 30-11		73	40,000	O5.5-6I-II	12.33	36,800
VFTS 566		73	164,000	O3III(f*)	14.05	44,700
LH 64-16		72	160,000	ON2III(f*)	13.666	50,900
NGC 2044-W35		72	160,000	O4III	14.1	48,200
VFTS 216		72	164,000	O4V((fc))	14.389	44,700
ST2-1		71	160,000	O5.5III	14.3	44,100
VFTS 3		71	164,000	B1Ia+	11.56	21,000
			24,800	WN6h	11.18	42,000
Arches Cluster-F12		70	25,000	WN7-8	16.4	36,900
HD 15629		70	7,500	O4.5V((fc))	8.42	45,900
HD 37974		70	163,000	B0.5e	10.99	22,500			N135 is an emission nebula in Large Magellanic Cloud.
HD 93129 Ab		70	7,500	O2If*	7.31	44,000
M33 X-7 B		70	2,700,000	O	18.7	35,000
Sk -69° 194 A		70	160,000	B0I+WN	12.131	45,000
VFTS 125		69.6	164,000	F5	16.6	55,200
NGC 3109-1		69.1	4,347,000	O8I	19.33	35,150
HD 46150		69	5,200	O5V((f))z	6.73	44,000
HD 229059		69	3,000	B2Iabe	8.7	26,300
ST2-3		69	160,000	O5.5V	14.264	44,900
ST2-32		69	160,000	O5(f)np	13.903	45,400
W28-23		69	160,000	O3.5V(f+)	13.702	51,300
HD 93403 A		68.5	10,400	O5.5III(fc)var	8.27	39,300
HD 93130		68	10,000	O7II(f)	8.04	39,900
HM 1-8		68	11,000	O5III(f)	12.52	46,100
HSH95-47		68	163,000	O3III	14.72	43,500
HSH95-48		68	163,000	O3III	14.75	46,500
Westerhout 51-61		68	20,000		18.16	38,000
BAT99-93		67	165,000	O3If*	13.446	45,000
Sk -69° 200		67	160,000	B1I	11.18	26,300
Arches Cluster-F18		66.9	25,000	O4-6I	16.7	36,900
Arches Cluster-F4		66.4	25,000	WN7-8	15.63	36,800
Z15		66.1	11,986,000	B0.5	20.495	25,000
BAT99-59 A		66	165,000	WN4b+O8:	13.186	71,000
BAT99-104		66	165,000	O2If*/WN5	12.5	63,000
HD 5980 B		66	200,000	WN4+O7I:	11.31	45,000
HD 190429 A		66	7,800	O4If	6.63	46,000
LH 31-1003		66	160,000	O6Ib	13.186	41,900
LH 114-7		66	160,000	O2III(f*)+OV	13.66	50,000			N70 is an emission nebula in Large Magellanic Cloud.
Pismis 24-1SW		66	6,500		11.1	40,000
BAT99-126		65	165,000	WN2.5-3+B1V+O4V+O6.5V	13.166	71,000
HSH95-40		65	163,000	O2-3.5V	14.56	47,500
HSH95-58		65	163,000	O3III	14.8	47,500
HSH95-89		65	163,000		14.76	44,000
VFTS 63		65	164,000	O5III(n)(fc)+sec	14.4	42,200
VFTS 145		65	164,000	O8fp	14.3	39,800
VFTS 518		65	164,000	O3.5III(f*)	15.11	44,700
Westerhout 49-8		65	36,200	O3-O7V	15.617	40,700
BD+43° 3654		64.6	5,400	O4If	10.06	40,400
BAT99-129 A		64	165,000	MN3ha+O5V	14.701	79,000			DEM L294 is a H II region in Large Magellanic Cloud.
HSH95-50		64	163,000		14.65	47,000
Sk -69° 25		64	160,000	OB	11.886	43,600
Trumpler 27-23		64	3,900	B0.7Ia	10.09	27,500
Westerhout 49-5		64	36,200	O3-O5V	15.623	42,700
HD 46223		63	5,200	O4V((f))	7.28	46,000
HD 64568		63	16,000	O3V((f*))z	9.39	54,000
HD 303308		63	9,200	O4.5V((fc))	8.17	51,300
HR 6187 A		63	4,300	O3.5-4III(f*)+O6IV	5.54	46,500	Septenary
LH 10-3058		63	160,000	O3V((f*))	14.089	54,000
ST5-71		63	160,000	O4.5III	13.266	45,400
AB9		62	197,000	WN3ha	15.431	100,000			DEM S80 is a H II region in Small Magellanic Cloud.
Brey 32 B		62	165,000	WC4+O6III/V+O	12.32	43,600
HD 93160		62	8,000	O7III((f))	7.6	42,700
HSH95-35		62	163,000	O3V	14.43	47,500
LH 41-1017		62	160,000	B1	12.266	42,700
Mercer 30-6a A		62	40,000	Ofpe/WN9	10.39	29,900
ST4-18		62	160,000	O5If	13.639	44,800
VFTS 664		62	164,000	O7II(f)	13.937	39,900
HD 229196		61.6	5,000	O6II(f)	8.59	40,900
AB8 B		61	197,000	WO4+O4V	12.83	45,000
BAT99-79 A		61	165,000	WN7ha+OB	13.486	42,000
HD 5980 A		61	200,000	WN4+O7I:	11.31	21,000–53,000
LH 41-18		61	160,000	O8.5V((f))	12.586	38,500
Mercer 30-9 A		61	40,000	O9-7I-III	12.25	34,500
ST5-25		61	160,000	O5-6V((f))z	13.551	48,600
VFTS 422		61	164,000	O4III(f)	15.14	39,800
WR 102hb		61	26,000	WN9	13.9	25,100
Sk -67° 166		60.68	160,000	O4Ia	12.22	41,800			GKK-A144 is a stellar association in Large Magellanic Cloud.
Sk -67° 167		60.68	160,000	O4If+n	12.586	41,800
Sk -71° 46		60.68	160,000	OB	13.241	41,800			BSDL 2242 is a star cluster in Large Magellanic Cloud.
Brey 10		60	165,000	WC	12.69	117,000
Brey 94 A		60	165,000	WR	12.996	83,000
Brey 95a A		60	165,000	G:	12.2	83,000
HSH95-55		60	163,000	O3V	14.74	47,500
Mercer 30-7 A		60	40,000	WN6	11.516	41,400
R134		60	164,000	WN6h	12.75	39,800
R142		60	164,000	B0Ia	11.82	18,000
R143		60	160,000	F7Ia	12.014	18,000–36,000
Sk -69° 142a		60	160,000	WN10h	11.093	34,000
Sk -69° 259		60	160,000	Be	11.93	23,000
Var 83		60	3,000,000	LBV	16.027	18,000–37,000
VFTS 430		60	164,000	B0.5Ia+((n))Nwk	15.11	24,500

A few notable large stars with masses less than 60 Solar mass 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.

Lambda Cephei		51.4	3,100	5.05	36,000
τ Canis Majoris Aa		50	5,120	4.89	32,000
Theta Muscae Ab		44	7,400	5.53	33,000
θ2 Orionis A		39	1,500	5.02	34,900
α Camelopardalis		37.6	6,000	4.29	29,000
P Cygni		37	5,100	4.82	18,700			IC 4996 is an open cluster in Cygnus OB1.
ζ1 Scorpii		36 - 53	8,210	4.705	17,200
Alnitak Aa		33	1,260	2.08	29,500
θ1 Orionis C1		33	1,340	5.13	39,000
κ Cassiopeiae		33	4,000	4.16	23,500
Mu Normae		33	3,260	4.91	28,000
Eta Carinae B		30	7,500	4.3	37,200
Gamma Velorum B		28.5	1,230	1.83	35,000
Alnilam			1,250	1.69	25,000
Meissa A		27.9	1,300	3.54	37,700
Xi Persei		26.1	1,200	4.04	35,000
Zeta Puppis			1,080	2.25	40,000			Vela R2 is a OB association in Vela Molecular Ridge.
WR 79a		24.4	5,600	5.77	35,000
Mintaka Aa1		24	1,200	2.5	29,500
ι Orionis Aa1		23.1	1,340	2.77	32,500
κ Crucis		23	7,500	5.98	16,300
WR 78		22	4,100	6.48	50,100
ο2 Canis Majoris		21.4	2,800	3.043	15,500
Rigel A		21	860	0.13	12,100
ζ Ophiuchi		20.2	370	2.569	34,000
υ Orionis		20	2,900	4.618	33,400
σ Orionis Aa		18	1,260	4.07	35,000
Mu Columbae		16	1,300	5.18	33,000
Saiph		15.5	650	2.09	26,500
Sigma Cygni		15	3,260	4.233	10,800
θ Carinae A		14.9	460	2.76	31,000
θ2 Orionis B		14.8	1,500	6.38	29,300
Zeta Persei		14.5	750	2.86	20,800
σ Orionis B		14	1,260	4.07	31,000
β Canis Majoris		13.5	490	1.985	23,200
ε Persei A		13.5	640	2.88	26,500
ι Orionis Aa2		13.1	1,340	2.77	27,000
δ Scorpii A		13	440	2.307	27,400
σ Orionis Ab		13	1,260	4.07	29,000
Theta Muscae Aa		11.5	7,400	5.53	83,000
Gamma Velorum A		9	1,230	1.83	57,000
ρ Ophiuchi A		8.7	360	4.63	22,000
Bellatrix		7.7	250	1.64	21,800
Antares B		7.2	550	5.5	18,500
Lambda Tauri A		7.18	480	3.47	18,700
Delta Persei		7	520	3.01	14,900
Psi Persei		6.2	580	4.31	16,000
Alpha Pavonis Aa		5.91	180	1.94	17,700
Alcyone		5.9	440	2.87	12,300
γ Canis Majoris		5.6	440	4.1	13,600
η Canis Majoris		5.5 or 9.5	2,000	2.45	15,000
ο Velorum		5.5	490	3.6	16,200
ο Aquarii		4.2	440	4.71	13,500
Nu Fornacis		3.65	370	4.69	13,400
Phi Eridani		3.55	150	3.55	13,700
η Chamaeleontis		3.2	310	5.453	12,500
ε Chamaeleontis		2.87	360	4.91	10,900
τ1 Aquarii		2.68	320	5.66	10,600
Epsilon Hydri		2.64	150	4.12	11,000
Beta Tucanae		2.5	140	4.37	10,600
Sun		1	0.0000158	−26.744	5,772		target="_blank" rel="nofollow" /a>

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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 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
• Intermediate-mass black holes range from 100 to
• Supermassive black holes are in the range of millions or billions .

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See also

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Footnotes

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External links

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