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{{short description|Black hole formed by a collapsed star}}{{distinguish|black hole star}}{{Use dmy dates|date=April 2020}}File:Artist’s impression of the black hole inside NGC 300 X-1 (ESO 1004a).jpg|right|thumb|upright=1.5|Artist's impression of a stellar-mass black hole (left) in the spiral galaxy NGC 300; it is associated with a Wolf–Rayet starWolf–Rayet starA stellar black hole (or stellar-mass black hole) is a black hole formed by the gravitational collapse of a star.JOURNAL , They have masses ranging from about 5 to several tens of solar masses.ARXIV, hep-ph/0511217, Hughes, Scott A., Trust but verify: The case for astrophysical black holes, 2005, They are the remnants of supernova explosions, which may be observed as a type of gamma ray burst. These black holes are also referred to as collapsars.

Properties

By the no-hair theorem, a black hole can only have three fundamental properties: mass, electric charge, and angular momentum. The angular momentum of a stellar black hole is due to the conservation of angular momentum of the star or objects that produced it.The gravitational collapse of a star is a natural process that can produce a black hole. It is inevitable at the end of the life of a massive star when all stellar energy sources are exhausted. If the mass of the collapsing part of the star is below the Tolman–Oppenheimer–Volkoff (TOV) limit for neutron-degenerate matter, the end product is a compact star – either a white dwarf (for masses below the Chandrasekhar limit) or a neutron star or a (hypothetical) quark star. If the collapsing star has a mass exceeding the TOV limit, the crush will continue until zero volume is achieved and a black hole is formed around that point in space.The maximum mass that a neutron star can possess before further collapsing into a black hole is not fully understood. In 1939, it was estimated at 0.7 solar masses, called the TOV limit. In 1996, a different estimate put this upper mass in a range from 1.5 to 3 solar masses.JOURNAL, I., Bombaci, 1996, The Maximum Mass of a Neutron Star, Astronomy and Astrophysics, 305, 871–877, 1996A&A...305..871B, The maximum observed mass of neutron stars is about {{solar mass|2.14}} for PSR J0740+6620 discovered in September, 2019.JOURNAL, Cromartie, H. T., Fonseca, E., Ransom, S. M., Demorest, P. B., Arzoumanian, Z., Blumer, H., Brook, P. R., DeCesar, M. E., Dolch, T., 2019-09-16, Relativistic Shapiro delay measurements of an extremely massive millisecond pulsar, Nature Astronomy, 4, 72–76, en, 10.1038/s41550-019-0880-2, 2397-3366, 2020NatAs...4...72C, 1904.06759, 118647384, In the theory of general relativity, a black hole could exist of any mass. The lower the mass, the higher the density of matter has to be in order to form a black hole. (See, for example, the discussion in Schwarzschild radius, the radius of a black hole.) There are no known stellar processes that can produce black holes with mass less than a few times the mass of the Sun. If black holes that small exist, they are most likely primordial black holes. Until 2016, the largest known stellar black hole was {{val|15.65|1.45}} solar masses.JOURNAL, 10.1038/449799a, Black holes go extragalactic, 2007, Bulik, Tomasz, Nature, 449, 7164, 799–801, 17943114, 4389109, free, In September 2015, a rotating black hole of {{val|62|4}} solar masses was discovered by gravitational waves as it formed in a merger event of two smaller black holes.JOURNAL, Observation of Gravitational Waves from a Binary Black Hole Merger, Physical Review Letters, 116, 6, 061102, 2016, 10.1103/PhysRevLett.116.061102, 26918975, Abbott, BP, et al, 1602.03837, 2016PhRvL.116f1102A, 124959784, {{As of|2020|06}}, the binary system 2MASS J05215658+4359220 was reportedJOURNAL, Thompson, Todd, A noninteracting low-mass black hole–giant star binary system, Science, 1 November 2019, 366, 6465, 637–640, 10.1126/science.aau4005, 31672898,weblink 1806.02751, 2019Sci...366..637T, 207815062, 3 June 2020, 11 September 2020,weblink live, to host the smallest-mass black hole currently known to science, with a mass 3.3 solar masses and a diameter of only 19.5 kilometers. There is observational evidence for two other types of black holes, which are much more massive than stellar black holes. They are intermediate-mass black holes (in the center of globular clusters) and supermassive black holes in the center of the Milky Way and other galaxies.

X-ray compact binary systems

Stellar black holes in close binary systems are observable when the matter is transferred from a companion star to the black hole; the energy released in the fall toward the compact star is so large that the matter heats up to temperatures of several hundred million degrees and radiates in X-rays. The black hole, therefore, is observable in X-rays, whereas the companion star can be observed with optical telescopes. The energy release for black holes and neutron stars are of the same order of magnitude. Black holes and neutron stars are therefore often difficult to distinguish.The derived masses come from observations of compact X-ray sources (combining X-ray and optical data). All identified neutron stars have a mass below 3.0 solar masses; none of the compact systems with a mass above 3.0 solar masses display the properties of a neutron star. The combination of these facts makes it more and more likely that the class of compact stars with a mass above 3.0 solar masses are in fact black holes.Note that this proof of the existence of stellar black holes is not entirely observational but relies on theory: we can think of no other object for these massive compact systems in stellar binaries besides a black hole. A direct proof of the existence of a black hole would be if one actually observes the orbit of a particle (or a cloud of gas) that falls into the black hole.

Black hole kicks

The large distances above the galactic plane achieved by some binaries are the result of black hole natal kicks. The velocity distribution of black hole natal kicks seems similar to that of neutron star kick velocities. One might have expected that it would be the momenta that were the same with black holes receiving lower velocity than neutron stars due to their higher mass but that doesn't seem to be the case,JOURNAL, 1203.3077, 10.1111/j.1365-2966.2012.21549.x, Investigating stellar-mass black hole kicks, 2012, Repetto, Serena, Davies, Melvyn B., Sigurdsson, Steinn, Monthly Notices of the Royal Astronomical Society, 425, 4, 2799–2809, 2012MNRAS.425.2799R, 119245969, which may be due to the fall-back of asymmetrically expelled matter increasing the momentum of the resulting black hole.JOURNAL, 1306.0007, 10.1093/mnras/stt1106, Natal kicks of stellar mass black holes by asymmetric mass ejection in fallback supernovae, 2013, Janka, Hans-Thomas, Monthly Notices of the Royal Astronomical Society, 434, 2, 1355–1361, 2013MNRAS.434.1355J, 119281755,

Mass gaps

It is predicted by some models of stellar evolution that black holes with masses in two ranges cannot be directly formed by the gravitational collapse of a star. These are sometimes distinguished as the "lower" and "upper" mass gaps, roughly representing the ranges of 2 to 5 and 50 to 150 solar masses ({{Solar mass}}), respectively.JOURNAL, 10.3847/2041-8213/ab3800, Binary Black Hole Population Properties Inferred from the First and Second Observing Runs of Advanced LIGO and Advanced Virgo, 2019, Abbott, B. P., Abbott, R., Abbott, T. D., Abraham, S., Acernese, F., Ackley, K., Adams, C., Adhikari, R. X., Adya, V. B., Affeldt, C., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Allen, G., Allocca, A., Aloy, M. A., Altin, P. A., Amato, A., Ananyeva, A., Anderson, S. B., Anderson, W. G., Angelova, S. V., Antier, S., Appert, S., Arai, K., Araya, M. C., The Astrophysical Journal, 882, 2, L24, 1811.12940, 2019ApJ...882L..24A, 119216482,weblink 29, 20 March 2020, 11 September 2020,weblink live, free, Another range given for the upper gap is 52 to 133 {{Solar mass}}.JOURNAL, Woosley, S.E., Pulsational Pair-instability Supernovae, The Astrophysical Journal, 836, 2, 2017, 244, 10.3847/1538-4357/836/2/244, 1608.08939, 2017ApJ...836..244W, 119229139, free, {{Solar mass|150}} has been regarded as the upper mass limit for stars in the current era of the universe.JOURNAL, Figer, D.F., An upper limit to the masses of stars, Nature, 434, 7030, 2005, 192–194, 10.1038/nature03293, 15758993, astro-ph/0503193, 2005Natur.434..192F, 4417561,

Lower mass gap

A lower mass gap is suspected on the basis of a scarcity of observed candidates with masses within a few solar masses above the maximum possible neutron star mass. The existence and theoretical basis for this possible gap are uncertain.JOURNAL, Kreidberg, Laura, Bailyn, Charles D., Farr, Will M., Kalogera, Vicky, Mass Measurements of Black Holes in X-Ray Transients: Is There a Mass Gap?, The Astrophysical Journal, 757, 1, 2012, 36, 0004-637X, 10.1088/0004-637X/757/1/36, 1205.1805, 2012ApJ...757...36K, 118452794, The situation may be complicated by the fact that any black holes found in this mass range may have been created via the merging of binary neutron star systems, rather than stellar collapse.JOURNAL, Safarzadeh, Mohammadtaher, Hamers, Adrian S., Loeb, Abraham, Berger, Edo, Formation and Merging of Mass Gap Black Holes in Gravitational-wave Merger Events from Wide Hierarchical Quadruple Systems, The Astrophysical Journal, 888, 1, 2019, L3, 2041-8213, 10.3847/2041-8213/ab5dc8, 1911.04495, 208527307, free, The LIGO/Virgo collaboration has reported three candidate events among their gravitational wave observations in run O3 with component masses that fall in this lower mass gap. There has also been reported an observation of a bright, rapidly rotating giant star in a binary system with an unseen companion emitting no light, including x-rays, but having a mass of {{val|3.3|+2.8|-0.7}} solar masses. This is interpreted to suggest that there may be many such low-mass black holes that are not currently consuming any material and are hence undetectable via the usual x-ray signature.JOURNAL, Thompson, Todd A., Kochanek, Christopher S., Stanek, Krzysztof Z., Badenes, Carles, Post, Richard S., Jayasinghe, Tharindu, Latham, David W., Bieryla, Allyson, Esquerdo, Gilbert A., Berlind, Perry, Calkins, Michael L., Tayar, Jamie, Lindegren, Lennart, Johnson, Jennifer A., Holoien, Thomas W.-S., Auchettl, Katie, Covey, Kevin, A noninteracting low-mass black hole–giant star binary system, Science, 366, 6465, 2019, 637–640, 0036-8075, 10.1126/science.aau4005, 31672898, 1806.02751, 2019Sci...366..637T, 207815062,

{{anchor|Upper mass gap}} Upper mass gap

The upper mass gap is predicted by comprehensive models of late-stage stellar evolution. It is expected that with increasing mass, supermassive stars reach a stage where a pair-instability supernova occurs, during which pair production, the production of free electrons and positrons in the collision between atomic nuclei and energetic gamma rays, temporarily reduces the internal pressure supporting the star's core against gravitational collapse.JOURNAL, Rakavy, G., Shaviv, G., Instabilities in Highly Evolved Stellar Models, The Astrophysical Journal, June 1967, 148, 803, 10.1086/149204, 1967ApJ...148..803R, free, This pressure drop leads to a partial collapse, which in turn causes greatly accelerated burning in a runaway thermonuclear explosion, resulting in the star being blown completely apart without leaving a stellar remnant behind.JOURNAL, Fraley, Gary S., Supernovae Explosions Induced by Pair-Production Instability, Astrophysics and Space Science, 1968, 2, 1, 96–114, 10.1007/BF00651498, 1968Ap&SS...2...96F, 122104256,weblink 25 February 2020, 1 December 2019,weblink live, Pair-instability supernovae can only happen in stars with a mass range from around 130 to 250 solar masses ({{Solar mass}}) (and low to moderate metallicity (low abundance of elements other than hydrogen and helium – a situation common in Population III stars)). However, this mass gap is expected to be extended down to about 45 solar masses by the process of pair-instability pulsational mass loss, before the occurrence of a "normal" supernova explosion and core collapse.JOURNAL, Farmer, R., Renzo, M., de Mink, S. E., Selma de Mink, Marchant, P., Justham, S., Mind the Gap: The Location of the Lower Edge of the Pair-instability Supernova Black Hole Mass Gap, The Astrophysical Journal, 887, 1, 2019, 53, 1538-4357, 10.3847/1538-4357/ab518b, 1910.12874, 2019ApJ...887...53F, 204949567,weblink 20 March 2020, 6 May 2020,weblink live, free, In nonrotating stars the lower bound of the upper mass gap may be as high as 60 {{Solar mass}}.JOURNAL, Mapelli, M., Spera, M., Montanari, E., Limongi, M., Chieffi, A., Giacobbo, N., Bressan, A., Bouffanais, Y., Impact of the Rotation and Compactness of Progenitors on the Mass of Black Holes, The Astrophysical Journal, 888, 2, 2020, 76, 10.3847/1538-4357/ab584d, 1909.01371, 2020ApJ...888...76M, 213050523, free, The possibility of direct collapse into black holes of stars with core mass > 133 {{Solar mass}}, requiring total stellar mass of > 260 {{Solar mass}} has been considered, but there may be little chance of observing such a high-mass supernova remnant; i.e., the lower bound of the upper mass gap may represent a mass cutoff. Observations of the LB-1 system of a star and unseen companion were initially interpreted in terms of a black hole with a mass of about 70 solar masses, which would be excluded by the upper mass gap. However, further investigations have weakened this claim.Black holes may also be found in the mass gap through mechanisms other than those involving a single star, such as the merger of black holes.

Candidates

{{see also|List of black holes|List of nearest known black holes}}Our Milky Way galaxy contains several stellar-mass black hole candidates (BHCs) which are closer to us than the supermassive black hole in the galactic center region. Most of these candidates are members of X-ray binary systems in which the compact object draws matter from its partner via an accretion disk. The probable black holes in these pairs range from three to more than a dozen solar masses.JOURNAL, astro-ph/0612312, 10.1017/S1743921307004590, Observational evidence for stellar-mass black holes, 2006, Casares, Jorge, Proceedings of the International Astronomical Union, 2, 3–12, 119474341, JOURNAL, M.R., Garcia, etal, Resolved Jets and Long Period Black Hole Novae, Astrophys. J., 2003, 591, 388–396, 10.1086/375218, astro-ph/0302230, 17521575, ARXIV, astro-ph/0306213, McClintock, Jeffrey E., Remillard, Ronald A., Black Hole Binaries, 2003, {| class="wikitable sortable"! rowspan="2" | Name ! colspan="2" | Mass (solar masses)! rowspan="2" | Orbital period(days) ! rowspan="2" style="line-height:120%" | DistancefromEarth (ly) ! rowspan="2" | CelestialCoordinatesICRS coordinates obtained from SIMBAD. Format: right ascension (hh:mm:ss) ±declination (dd:mm:ss).! BHC! Companion|Gaia BH3|32.70 Â± 0.82|0.76 Â± 0.05|4,253.1 Â± 98.5|{{0}}1926|19:39:19 +14:55:54

Cygnus X-1>Cyg X-1

21.2 ± 2.2MILLER-JONES >FIRST1=JAMES C. A.

FIRST2=ARASH

FIRST3=JEROME A.

FIRST4=ILYA

FIRST5=LIJUN

FIRST6=THOMAS J.

FIRST7=COENRAAD J.

FIRST8=XUESHAN

FIRST9=JANUSZ

FIRST10=MARK J.

FIRST11=PHIL

FIRST12=XUEYING

FIRST13=DO-YOUNG

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FIRST15=VICTORIA

TITLE=CYGNUS X-1 CONTAINS A 21–SOLAR MASS BLACK HOLE—IMPLICATIONS FOR MASSIVE STAR WINDS

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LAST26=WILMS

40.6

7.1}}

5.6

{{0}}6000...8000

19:58:22 +35:12:06

GRS 1915+105/V1487 Aql >				|19:15:12 +10:56:44

V404 Cyg >					JOURNAL=THE ASTROPHYSICAL JOURNAL LETTERS	ISSUE=2	ARXIV=0910.5253	LAST3=DHAWAN	DOI = 10.1088/0004-637X/706/2/L230	S2CID=17750440,	20:24:04 +33:52:03

A0620-00/V616 Mon >				| 06:22:44 −00:20:45

XTE J1650-500 >

FIRST1=N.

FIRST2=L.

JOURNAL=THE ASTROPHYSICAL JOURNAL

ISSUE=1

DOI=10.1088/0004-637X/699/1/453

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LAST4=CORBEL

DATE=2004

VOLUME=616

PAGES=376–382

DOI=10.1086/424892

S2CID=13933140,

10763

16:50:01 −49:57:45

|Gaia BH1|9.62 Â± 0.18|0.93 Â± 0.05|185.59 Â± 0.05|{{0}}1560|17:28:41 −00:34:52

XTE J1550-564/V381 Nor >				|15:50:59 −56:28:36

4U 1543-475/IL Lupi >				| 15:47:09 −47:40:10

|Gaia BH2|8.94 Â± 0.34|1.07 Â± 0.19|1,276.7 Â± 0.6|{{0}}3800|13:50:17 −59:14:20

MAXI J1305-704MATA SáNCHEZ

LAST2=RAU

LAST3=ÁLVAREZ HERNáNDEZ

LAST4=VAN GRUNSVEN

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ISSN=0035-8711,

8.9

1.0}}|0.43 Â± 0.16|0.394 Â± 0.004|24500|13:06:55 −70:27:05

BW Circini>GS 1354-64 (BW Cir)CASARES >FIRST1=J.

FIRST2=J. A.

FIRST3=C.

FIRST4=T.

FIRST5=J. M.

FIRST6=J. E.

FIRST7=M. R.

FIRST8=I. G.

FIRST9=P. A.

FIRST10=R. P.

FIRST11=R. A.

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JOURNAL=THE ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES

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DOI=10.1088/0067-0049/181/1/238

ISSN=0067-0049, |7.9 Â± 0.5|1.1 Â± 0.1|2.5445|>81500|13:58:10 −64:44:06

XTE J1859+226>XTE J1859+226 (V406 Vul)YANES-RIZO >FIRST1=I. V.

FIRST2=M. A. P.

FIRST3=J.

FIRST4=S. E.

FIRST5=T.

FIRST6=P.

FIRST7=M.

FIRST8=F.

FIRST9=P. G.

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FIRST11=R.

TITLE=A REFINED DYNAMICAL MASS FOR THE BLACK HOLE IN THE X-RAY TRANSIENT XTE J1859+226

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ISSUE=1

DOI=10.1093/MNRAS/STAC2719

BIBCODE=2022MNRAS.517.1476Y, 0035-8711, |7.8 Â± 1.9|0.55 Â± 0.16|0.276 Â± 0.003||18:58:42 +22:39:29

HD 130298MAHY

LAST2=SANA

LAST3=SHENAR

LAST4=SEN

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LAST7=ABDUL-MASIH

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NGC 3201 21859>NGC 3201 #21859GIESERS >FIRST1=BENJAMIN

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PAGES=L12

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GS 2000+25/QZ Vul >				| 20:02:50 +25:14:11

V4641 Sagittarii>XTE J1819-254/V4641 Sgr	7.1 Â± 0.3	5...8	2.82	24000...40000OROSZ >DISPLAY-AUTHORS=ETAL	JOURNAL=THE ASTROPHYSICAL JOURNAL	VOLUME=555	PAGES=489	ARXIV=ASTRO-PH/0103045V1	S2CID=50248739,	18:19:22 −25:24:25

LB-1 (disputed)SHENAR, T.

AUTHOR3=ABDUL-MASIH, M.

AUTHOR5=MARCHANT, P.

AUTHOR7=BOWMAN, D. M.

AUTHOR9=HAWCROFT, C.

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7 Â± 2

1.5 Â± 0.4

78.7999 Â± 0.0097

15000CHINESE ACADEMY OF SCIENCE >AUTHOR-LINK=CHINESE ACADEMY OF SCIENCE

TITLE=CHINESE ACADEMY OF SCIENCES LEADS DISCOVERY OF UNPREDICTED STELLAR BLACK HOLE

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ARCHIVE-DATE=28 NOVEMBER 2019

WORK=EUREKALERT!,

06:11:49 +22:49:32LIU, JIFENG >DISPLAY-AUTHORS=ET AL.

TITLE=A WIDE STAR–BLACK-HOLE BINARY SYSTEM FROM RADIAL-VELOCITY MEASUREMENTS

NATURE (JOURNAL)>NATURE

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S2CID=208310287,

|GRS 1124-683/Nova Muscae 1991/GU Mus

			| 11:26:27 −68:40:32

H 1705-25/Nova Ophiuchi 1977/V2107 OphDASHWOOD BROWN

LAST2=GANDHI

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ISSN=0066-4146, |0.34 Â± 0.08|0.52125||17:08:15 −25:05:30

XTE J1118+480/KV UMa >				| 11:18:11 +48:02:13

MAXI J1820+070MIKOÅ‚AJEWSKA

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6.75

0.46}}|0.49 Â± 0.1|0.68549 Â± 0.00001|{{0}}9800|18:20:22 +07:11:07

GRO J1655-40/V1033 Sco >				| 16:54:00 −39:50:45

GX 339-4/V821 Ara >				| 17:02:50 −48:47:23

GRO J1719-24>			last1=Masetti | first1= N. |last2=Bianchini | first2=A. |last3=Bonibaker | first3=J. |last4=della Valle | first4=M. |last5=Vio | first5=R.|title=The superhump phenomenon in GRS 1716-249 (=X-Ray Nova Ophiuchi 1993)| journal=Astronomy and Astrophysics| volume=314|date=1996| pages= 123 | bibcode= 1996A&A...314..123M }}|| {{0}}8500 || 17:19:37 −25:01:03

NGC 3201 12560>NGC 3201 #12560|4.53 Â± 0.21|0.81 Â± 0.05|167.01 Â± 0.09|15700|10:17:37 −46:24:55

GRS 1009-45 /Nova Velorum 1993/MM VelorumFILIPPENKO	LAST2=LEONARD	LAST3=MATHESON	LAST4=LI	LAST5=MORAN	LAST6=RIESS	DATE=1999-08-01	URL=HTTPS://UI.ADSABS.HARVARD.EDU/ABS/1999PASP..111..969F	VOLUME=111	PAGES=969–979	ARXIV=ASTRO-PH/9904271	ISSN=0004-6280, |4.3 Â± 0.1|0.5...0.65|0.285206 Â±0.0000014|17200|10:13:36 −45:04:33

GRO J0422+32/V518 Per>				| 04:21:43 +32:54:27

Extragalactic

Candidates outside our galaxy come from gravitational wave detections:{| class="wikitable sortable"|+ Outside our galaxy!Name || BHC mass(solar masses)|| Companion mass(solar masses ) || Orbital period(days) || Distance from Earth(light years) || Location

GW190521 ({{Val>155	11}}) {{Solar mass}}	78	5}}2009.05461 >CLASS=ASTRO-PH.HE	TITLE=GW190521 AS A HIGHLY ECCENTRIC BLACK HOLE MERGER	YEAR=2020,	78	5}}|||

GW150914 (62 Â± 4) {{Solar mass}} >				|

|GW170104 (48.7 Â± 5) {{Solar mass}}|31.2 Â± 7|19.4 Â± 6| .|1.4 billion|

GW170814 ({{Val>53.2	2.5}}) {{Solar mass}}	30.5	3.0}}	25.3	4.2}}||1.8 billion|

|GW190412|29.7|8.4||2.4 billion||GW190814|22.2–24.3|2.50–2.67||||GW151226 (21.8 Â± 3.5) {{Solar mass}}|14.2 Â± 6|7.5 Â± 2.3|.|2.9 billion||GW170608

12	2}}|7 Â± 2||1.1 billion|

Candidates outside our galaxy from X-ray binaries:{| class="wikitable sortable"!Name !Host galaxy|| BHC mass(solar masses)|| Companion mass(solar masses ) || Orbital period(days) || Distance from Earth(light years)

IC 10 X-1LAYCOCK	LAST2=CAPPALLO	LAST3=MORO	DATE=2015-01-01	URL=HTTPS://UI.ADSABS.HARVARD.EDU/ABS/2015MNRAS.446.1399L	VOLUME=446	PAGES=1399–1410	ARXIV=1410.3417	ISSN=0035-8711, |IC 10|≥23.1 Â± 2.1|≥17|1.45175|2.15 million

NGC 300 X-1BINDER

LAST2=SY

LAST3=ERACLEOUS

LAST4=CHRISTODOULOU

LAST5=BHATTACHARYA

LAST6=CAPPALLO

LAST7=LAYCOCK

LAST8=PLUCINSKY

LAST9=WILLIAMS

DATE=2021-03-01

JOURNAL=THE ASTROPHYSICAL JOURNAL

ISSUE=1

DOI=10.3847/1538-4357/ABE6A9

ARXIV=2102.07065

ISSN=0004-637X, |NGC 300|17 Â± 4

26

5}}|1.3663375|6.5 million

|M33 X-7|Triangulum Galaxy|15.65 Â± 1.45|70 Â± 6.9|3.45301 Â± 0.00002|2.7 million

LMC X-1OROSZ

LAST2=STEEGHS

LAST3=MCCLINTOCK

LAST4=TORRES

LAST5=BOCHKOV

LAST6=GOU

LAST7=NARAYAN

LAST8=BLASCHAK

LAST9=LEVINE

LAST10=REMILLARD

LAST11=BAILYN

LAST12=DWYER

LAST13=BUXTON

DATE=2009-05-01

URL=HTTPS://UI.ADSABS.HARVARD.EDU/ABS/2009APJ...697..573O

VOLUME=697

PAGES=573–591

ARXIV=0810.3447

ISSN=0004-637X, |Large Magellanic Cloud|10.91 Â± 1.41|31.79 Â± 3.48|3.9094 Â± 0.0008

LAST2=GALLI

LAST3=TREVES

LAST4=CHIAPPETTI

LAST5=DAL FIUME

LAST6=CORONGIU

LAST7=BELLONI

LAST8=FRONTERA

LAST9=KUULKERS

LAST10=STELLA

DATE=2001-03-01

URL=HTTPS://UI.ADSABS.HARVARD.EDU/ABS/2001APJS..133..187H

VOLUME=133

PAGES=187–193

ARXIV=ASTRO-PH/0009231

ISSN=0067-0049,

LMC X-3OROSZ

LAST2=STEINER

LAST3=MCCLINTOCK

LAST4=BUXTON

LAST5=BAILYN

LAST6=STEEGHS

LAST7=GUBERMAN

LAST8=TORRES

DATE=2014-10-01

URL=HTTPS://UI.ADSABS.HARVARD.EDU/ABS/2014APJ...794..154O

VOLUME=794

PAGES=154

ARXIV=1402.0085

ISSN=0004-637X, |Large Magellanic Cloud|6.98 Â± 0.56|3.63 Â± 0.57|1.704808|157,000

The disappearance of N6946-BH1 following a failed supernova in NGC 6946 may have resulted in the formation of a black hole.ARXIV, Adams, S. M., Kochanek, C. S, Gerke, J. R., Stanek, K. Z., Dai, X., The search for failed supernovae with the Large Binocular Telescope: conformation of a disappearing star, 9 September 2016, 1609.01283v1, astro-ph.SR,

See also

• Black holes in fiction
• Supermassive black hole
• Rogue black hole
• Primordial black hole

References

{{reflist}}

External links

{{wiktionary|collapsar}}

• Black Holes: Gravity's Relentless Pull {{Webarchive|url=https://web.archive.org/web/20080517091731weblink |date=17 May 2008 }} Award-winning interactive multimedia Web site about the physics and astronomy of black holes from the Space Telescope Science Institute
• weblink" title="web.archive.org/web/20021028112105weblink">Black hole diagrams
• JOURNAL, astro-ph/0307307, Ziółkowski, Janusz, Black Hole Candidates, Frontier Objects in Astrophysics and Particle Physics, 2003, 411, 2003foap.conf..411Z,
• Heaviest Stellar Black Hole Discovered in Nearby Galaxy, Newswise, 17-Oct-2007

{{Black holes}}{{Star}}{{Neutron star}}{{supernovae}}