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== Black hole kicks ==
== Black hole kicks ==
The large distances above the [[galactic plane]] achieved by some [[X-ray binary|binaries]] are the result of black hole natal kicks. The velocity distribution of black hole natal kicks seems similar to that of [[pulsar kick|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,<ref>{{Cite journal |arxiv = 1203.3077|doi = 10.1111/j.1365-2966.2012.21549.x|title = Investigating stellar-mass black hole kicks|year = 2012|last1 = Repetto|first1 = Serena|last2 = Davies|first2 = Melvyn B.|last3 = Sigurdsson|first3 = Steinn|journal = Monthly Notices of the Royal Astronomical Society|volume = 425|issue = 4|pages = 2799–2809|bibcode = 2012MNRAS.425.2799R|s2cid = 119245969}}</ref> which may be due to the fall-back of asymmetrically expelled matter increasing the momentum of the resulting black hole.<ref>{{Cite journal |arxiv = 1306.0007|doi = 10.1093/mnras/stt1106|title = Natal kicks of stellar mass black holes by asymmetric mass ejection in fallback supernovae|year = 2013|last1 = Janka|first1 = Hans-Thomas|journal = Monthly Notices of the Royal Astronomical Society|volume = 434|issue = 2|pages = 1355–1361|bibcode = 2013MNRAS.434.1355J|s2cid = 119281755}}</ref>
The large distances above the [[galactic plane]] achieved by some [[X-ray binary|binaries]] are the result of black hole natal kicks. The velocity distribution of black hole natal kicks seems similar to that of [[pulsar kick|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,<ref>{{Cite journal |arxiv = 1203.3077|doi = 10.1111/j.1365-2966.2012.21549.x|title = Investigating stellar-mass black hole kicks|year = 2012|last1 = Repetto|first1 = Serena|last2 = Davies|first2 = Melvyn B.|last3 = Sigurdsson|first3 = Steinn|journal = Monthly Notices of the Royal Astronomical Society|volume = 425|issue = 4|pages = 2799–2809| doi-access=free |bibcode = 2012MNRAS.425.2799R|s2cid = 119245969}}</ref> which may be due to the fall-back of asymmetrically expelled matter increasing the momentum of the resulting black hole.<ref>{{Cite journal |arxiv = 1306.0007|doi = 10.1093/mnras/stt1106|title = Natal kicks of stellar mass black holes by asymmetric mass ejection in fallback supernovae|year = 2013|last1 = Janka|first1 = Hans-Thomas|journal = Monthly Notices of the Royal Astronomical Society|volume = 434|issue = 2|pages = 1355–1361| doi-access=free |bibcode = 2013MNRAS.434.1355J|s2cid = 119281755}}</ref>


== Mass gaps ==
== Mass gaps ==
Line 49: Line 49:
The upper mass gap is predicted by comprehensive models of late-stage stellar evolution. It is expected that with increasing mass, [[hypergiant|supermassive star]]s reach a stage where a [[pair-instability supernova]] occurs, during which [[pair production]], the production of free [[electron]]s and [[positron]]s in the collision between [[atomic nuclei]] and energetic [[gamma ray]]s, temporarily reduces the internal pressure supporting the star's core against gravitational collapse.<ref>{{cite journal |last1=Rakavy |first1=G. |last2=Shaviv |first2=G. |title=Instabilities in Highly Evolved Stellar Models |journal=The Astrophysical Journal |date=June 1967 |volume=148 |pages=803 |doi=10.1086/149204|bibcode=1967ApJ...148..803R |doi-access=free }}</ref> This pressure drop leads to a partial collapse, which in turn causes greatly accelerated burning in a [[thermal runaway|runaway]] thermonuclear explosion, resulting in the star being blown completely apart without leaving a stellar remnant behind.<ref>{{cite journal|last=Fraley|first=Gary S.|title=Supernovae Explosions Induced by Pair-Production Instability|journal=[[Astrophysics and Space Science]]|date=1968|volume=2|issue=1|pages=96–114|doi=10.1007/BF00651498|bibcode=1968Ap&SS...2...96F|s2cid=122104256|url=https://thesis.library.caltech.edu/9293/1/Fraley_gs_1967.pdf|access-date=25 February 2020|archive-date=1 December 2019|archive-url=https://web.archive.org/web/20191201004915/https://thesis.library.caltech.edu/9293/1/Fraley_gs_1967.pdf|url-status=live}}</ref>
The upper mass gap is predicted by comprehensive models of late-stage stellar evolution. It is expected that with increasing mass, [[hypergiant|supermassive star]]s reach a stage where a [[pair-instability supernova]] occurs, during which [[pair production]], the production of free [[electron]]s and [[positron]]s in the collision between [[atomic nuclei]] and energetic [[gamma ray]]s, temporarily reduces the internal pressure supporting the star's core against gravitational collapse.<ref>{{cite journal |last1=Rakavy |first1=G. |last2=Shaviv |first2=G. |title=Instabilities in Highly Evolved Stellar Models |journal=The Astrophysical Journal |date=June 1967 |volume=148 |pages=803 |doi=10.1086/149204|bibcode=1967ApJ...148..803R |doi-access=free }}</ref> This pressure drop leads to a partial collapse, which in turn causes greatly accelerated burning in a [[thermal runaway|runaway]] thermonuclear explosion, resulting in the star being blown completely apart without leaving a stellar remnant behind.<ref>{{cite journal|last=Fraley|first=Gary S.|title=Supernovae Explosions Induced by Pair-Production Instability|journal=[[Astrophysics and Space Science]]|date=1968|volume=2|issue=1|pages=96–114|doi=10.1007/BF00651498|bibcode=1968Ap&SS...2...96F|s2cid=122104256|url=https://thesis.library.caltech.edu/9293/1/Fraley_gs_1967.pdf|access-date=25 February 2020|archive-date=1 December 2019|archive-url=https://web.archive.org/web/20191201004915/https://thesis.library.caltech.edu/9293/1/Fraley_gs_1967.pdf|url-status=live}}</ref>


Pair-instability [[supernova]]e 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.<ref name="FarmerRenzo2019">{{cite journal|last1=Farmer|first1=R.|last2=Renzo|first2=M.|last3=de Mink|first3=S. E.|author3-link=Selma de Mink|last4=Marchant|first4=P.|last5=Justham|first5=S.|title=Mind the Gap: The Location of the Lower Edge of the Pair-instability Supernova Black Hole Mass Gap|journal=The Astrophysical Journal|volume=887|issue=1|year=2019|pages=53|issn=1538-4357|doi=10.3847/1538-4357/ab518b|arxiv=1910.12874|bibcode=2019ApJ...887...53F|s2cid=204949567|url=https://pure.uva.nl/ws/files/44945808/Mind_the_Gap.pdf|access-date=20 March 2020|archive-date=6 May 2020|archive-url=https://web.archive.org/web/20200506070134/https://pure.uva.nl/ws/files/44945808/Mind_the_Gap.pdf|url-status=live |doi-access=free }}</ref> In nonrotating stars the lower bound of the upper mass gap may be as high as 60 {{Solar mass}}.<ref name="Mapelli2020">{{cite journal|last1= Mapelli|first1=M.|last2= Spera|first2=M.|last3= Montanari|first3=E.|last4= Limongi|first4=M.|last5= Chieffi|first5=A.|last6= Giacobbo|first6=N.|last7= Bressan|first7=A.|last8= Bouffanais|first8=Y.|title= Impact of the Rotation and Compactness of Progenitors on the Mass of Black Holes |journal=The Astrophysical Journal |volume= 888|issue= 2|year= 2020|pages= 76|doi= 10.3847/1538-4357/ab584d|arxiv=1909.01371|bibcode=2020ApJ...888...76M|s2cid=213050523 |doi-access=free }}</ref> 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.<ref name="Woosley2017" />
Pair-instability [[supernova]]e 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.<ref name="FarmerRenzo2019">{{cite journal|last1=Farmer|first1=R.|last2=Renzo|first2=M.|last3=de Mink|first3=S. E.|author3-link=Selma de Mink|last4=Marchant|first4=P.|last5=Justham|first5=S.|title=Mind the Gap: The Location of the Lower Edge of the Pair-instability Supernova Black Hole Mass Gap|journal=The Astrophysical Journal|volume=887|issue=1|year=2019|pages=53|issn=1538-4357|doi=10.3847/1538-4357/ab518b|arxiv=1910.12874|bibcode=2019ApJ...887...53F|s2cid=204949567|url=https://pure.uva.nl/ws/files/44945808/Mind_the_Gap.pdf|access-date=20 March 2020|archive-date=6 May 2020|archive-url=https://web.archive.org/web/20200506070134/https://pure.uva.nl/ws/files/44945808/Mind_the_Gap.pdf|url-status=live |doi-access=free }}</ref> In nonrotating stars the lower bound of the upper mass gap may be as high as 60 {{Solar mass}}.<ref name="Mapelli2020">{{cite journal|last1= Mapelli|first1=M.|last2= Spera|first2=M.|last3= Montanari|first3=E.|last4= Limongi|first4=M.|last5= Chieffi|first5=A.|last6= Giacobbo|first6=N.|last7= Bressan|first7=A.|last8= Bouffanais|first8=Y.|title= Impact of the Rotation and Compactness of Progenitors on the Mass of Black Holes |journal=The Astrophysical Journal |volume= 888|issue= 2|year= 2020|pages= 76|doi= 10.3847/1538-4357/ab584d|arxiv=1909.01371|bibcode=2020ApJ...888...76M|s2cid=213050523 |doi-access=free }}</ref> 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.<ref name="Woosley2017" />


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.
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.
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Our [[Milky Way|Milky Way galaxy]] contains several stellar-mass black hole candidates (BHCs) which are closer to us than the supermassive black hole in the [[Sagittarius A*|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 mass]]es.<ref>{{Cite journal |arxiv = astro-ph/0612312|doi = 10.1017/S1743921307004590|title = Observational evidence for stellar-mass black holes|year = 2006|last1 = Casares|first1 = Jorge|journal = Proceedings of the International Astronomical Union|volume = 2|pages = 3–12|s2cid = 119474341}}</ref><ref>{{cite journal |first=M.R. |last=Garcia |display-authors=etal |title=Resolved Jets and Long Period Black Hole Novae |journal= Astrophys. J.|year=2003 |volume=591 |pages=388–396 |doi=10.1086/375218 |arxiv=astro-ph/0302230 |s2cid=17521575 }}</ref><ref>{{Cite arXiv |eprint = astro-ph/0306213|last1 = McClintock|first1 = Jeffrey E.|last2 = Remillard|first2 = Ronald A.|title = Black Hole Binaries|year = 2003}}</ref>
Our [[Milky Way|Milky Way galaxy]] contains several stellar-mass black hole candidates (BHCs) which are closer to us than the supermassive black hole in the [[Sagittarius A*|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 mass]]es.<ref>{{Cite journal |arxiv = astro-ph/0612312|doi = 10.1017/S1743921307004590|title = Observational evidence for stellar-mass black holes|year = 2006|last1 = Casares|first1 = Jorge|journal = Proceedings of the International Astronomical Union|volume = 2|pages = 3–12|s2cid = 119474341}}</ref><ref>{{cite journal |first=M.R. |last=Garcia |display-authors=etal |title=Resolved Jets and Long Period Black Hole Novae |journal= Astrophys. J.|year=2003 |volume=591 |pages=388–396 |doi=10.1086/375218 |arxiv=astro-ph/0302230 |s2cid=17521575 }}</ref><ref>{{Cite arXiv |eprint = astro-ph/0306213|last1 = McClintock|first1 = Jeffrey E.|last2 = Remillard|first2 = Ronald A.|title = Black Hole Binaries|year = 2003}}</ref>
{{sticky header}}

{| class="wikitable sortable"
{| class="wikitable sortable sticky-header-multi"
! rowspan="2" | Name
!Name || [[Black hole|BHC]] mass<br />([[solar mass]]es)|| Companion mass<br />(solar masses ) || [[Orbital period]]<br />(days) || Distance from Earth<br />([[light year]]s) || Location<ref name="ReferenceA">[[International Celestial Reference System|ICRS]] coordinates obtained from [[SIMBAD]]. Format: [[right ascension]] (hh:mm:ss) ±[[declination]] (dd:mm:ss).</ref>
! colspan="2" | Mass ([[solar mass]]es)
! rowspan="2" | [[Orbital period]]<br />(days)
! rowspan="2" style="line-height:120%" | Distance<br>from<br>Earth ([[light year|ly]])
! rowspan="2" | Celestial<br>Coordinates<ref name="ReferenceA">[[International Celestial Reference System|ICRS]] coordinates obtained from [[SIMBAD]]. Format: [[right ascension]] (hh:mm:ss) ±[[declination]] (dd:mm:ss).</ref>
|-
|-
! [[Black hole|BHC]]
|[[LB-1]] || 68 +11/-13<ref name="NAT-20191127">{{cite journal |author=Liu, Jifeng |display-authors=et al. |title=A wide star–black-hole binary system from radial-velocity measurements |date=27 November 2019 |journal=[[Nature (journal)|Nature]] |volume=575 |issue=7784 |pages=618–621 |doi=10.1038/s41586-019-1766-2 |pmid=31776491 |arxiv=1911.11989 |bibcode=2019Natur.575..618L |s2cid=208310287 }}</ref> || 8<ref name="EA-20191127a">{{cite web |author=Chinese Academy of Science |title=Chinese Academy of Sciences leads discovery of unpredicted stellar black hole |url=https://www.eurekalert.org/pub_releases/2019-11/caos-cao112519.php |date=27 November 2019 |work=[[EurekAlert!]] |access-date=29 November 2019 |author-link=Chinese Academy of Science |archive-date=28 November 2019 |archive-url=https://web.archive.org/web/20191128233834/https://www.eurekalert.org/pub_releases/2019-11/caos-cao112519.php |url-status=live }}</ref> || 78.9<ref name="NAT-20191127" /> ||15,000<ref name="EA-20191127a" /> || 06:11:49 +22:49:32<ref name="NAT-20191127" />
! Companion
|-
|-
|[[Gaia BH3]]
|[[A0620-00]]/[[V616 Mon]] || 11 ± 2 || 2.6–2.8 || 0.33 || 3,500 || 06:22:44 -00:20:45
|32.70&nbsp;±&nbsp;0.82
|0.76&nbsp;±&nbsp;0.05
|4,253.1&nbsp;±&nbsp;98.5
|{{0}}1926
|19:39:19&nbsp;+14:55:54
|-
|-
|[[Cygnus X-1|Cyg X-1]] || 21.2 ± 2.2<ref name=":0">{{cite journal |last1=Miller-Jones |first1=James C. A. |last2=Bahramian |first2=Arash |last3=Orosz |first3=Jerome A. |last4=Mandel |first4=Ilya |last5=Gou |first5=Lijun |last6=Maccarone |first6=Thomas J. |last7=Neijssel |first7=Coenraad J. |last8=Zhao |first8=Xueshan |last9=Ziółkowski |first9=Janusz |last10=Reid |first10=Mark J. |last11=Uttley |first11=Phil |last12=Zheng |first12=Xueying |last13=Byun |first13=Do-Young |last14=Dodson |first14=Richard |last15=Grinberg |first15=Victoria |date=5 March 2021 |title=Cygnus X-1 contains a 21–solar mass black hole—Implications for massive star winds |journal=Science |volume=371 |issue=6533 |pages=1046–1049 |arxiv=2102.09091 |bibcode=2021Sci...371.1046M |doi=10.1126/science.abb3363 |pmid=33602863 |s2cid=231951746 |last16=Jung |first16=Taehyun |last17=Kim |first17=Jeong-Sook |last18=Marcote |first18=Benito |last19=Markoff |first19=Sera |last20=Rioja |first20=María J. |last21=Rushton |first21=Anthony P. |last22=Russell |first22=David M. |last23=Sivakoff |first23=Gregory R. |last24=Tetarenko |first24=Alexandra J. |last25=Tudose |first25=Valeriu |last26=Wilms |first26=Joern}}</ref>|| {{Val|40.6|7.7|7.1}}<ref name=":0" /> || 5.6 || {{0}}6000...8000 || 19:58:22 +35:12:06
|[[GRO J1655-40]]/[[GRO J1655-40|V1033 Sco]] || 6.3 ± 0.3 || 2.6–2.8 || 2.8 || 5,000–11,000|| 16:54:00 -39:50:45
|-
|-
|[[XTE J1118+480]]/[[KV UMa]] || 6.8 ± 0.4 || 6−6.5 || 0.17 || 6,200 || 11:18:11 +48:02:13
|[[GRS 1915+105]]/V1487 Aql || 14&nbsp;±&nbsp;4.0 || ≈1 || 33.5 || 40000 ||19:15:12 +10:56:44
|-
|-
|[[V404 Cyg]] || 12&nbsp;±&nbsp;2 || 6.0 || 6.5 || {{0}}7800&nbsp;±&nbsp;460<ref>{{cite journal|title=The first accurate parallax distance to a black hole|author=Miller-Jones, J. A. C.|journal=The Astrophysical Journal Letters|volume=706|issue=2|page=L230|arxiv=0910.5253|last2=Jonker|last3=Dhawan|bibcode = 2009ApJ...706L.230M |doi = 10.1088/0004-637X/706/2/L230 |year=2009|s2cid=17750440}}</ref> || 20:24:04 +33:52:03
|[[Cygnus X-1|Cyg X-1]] || 11 ± 2|| ≥18 || 5.6 || 6,000–8,000 || 19:58:22 +35:12:06
|-
|-
|[[GRO J0422+32]]/[[V518 Per]] || 4 ± 1 || 1.1 || 0.21 || 8,500 || 04:21:43 +32:54:27
|[[A0620-00]]/V616 Mon || 11&nbsp;±&nbsp;2 || 2.6–2.8 || 0.33 || {{0}}3500 || 06:22:44 −00:20:45
|-
|-
|[[XTE J1650-500]] || 9.7&nbsp;±&nbsp;1.6<ref>{{cite journal |title=Determination of Black Hole Masses in Galactic Black Hole Binaries using Scaling of Spectral and Variability Characteristics |last1=Shaposhnikov |first1=N. |last2=Titarchuk |first2=L. |date=2009 |journal=The Astrophysical Journal |volume=699 |issue=1 |pages=453–468 |doi=10.1088/0004-637X/699/1/453 |arxiv=0902.2852v1 |bibcode=2009ApJ...699..453S |s2cid=18336866 }}</ref> || 5–10 || 0.32<ref>{{cite journal |title=Orbital Parameters for the Black Hole Binary XTE J1650–500 |display-authors=1 |last1=Orosz |first1=J.A. |last2=McClintock |first2=J.E. |last3=Remillard |first3=R.A. |last4=Corbel |first4=S. |date=2004 |journal=The Astrophysical Journal |volume=616 |issue=1 |pages=376–382 |bibcode=2004ApJ...616..376O |doi=10.1086/424892 |arxiv=astro-ph/0404343 |s2cid=13933140 }}</ref> || 10763||16:50:01 −49:57:45
|[[GRO J1719-24]] || {{sort|5|≥4.9}} || ~1.6 || possibly 0.6<ref name="Masetti1996">{{citation|
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 }}</ref> || 8,500 || 17:19:37 -25:01:03
|-
|-
|[[Gaia BH1]]
|[[GS 2000+25]]/[[QZ Vul]] || 7.5 ± 0.3 || 4.9–5.1 || 0.35 || 8,800 || 20:02:50 +25:14:11
|9.62&nbsp;±&nbsp;0.18
|0.93&nbsp;±&nbsp;0.05
|185.59&nbsp;±&nbsp;0.05
|{{0}}1560
|17:28:41 −00:34:52
|-
|-
|[[XTE J1550-564]]/V381 Nor || 9.6&nbsp;±&nbsp;1.2 || 6.0...7.5 || 1.5 || 17000 ||15:50:59 −56:28:36
|[[V404 Cyg]] || 12 ± 2 || 6.0 || 6.5 || 7,800 ± 460<ref>{{cite journal|title=The first accurate parallax distance to a black hole|author=Miller-Jones, J. A. C.|journal=The Astrophysical Journal Letters|volume=706|issue=2|page=L230|arxiv=0910.5253|last2=Jonker|last3=Dhawan|bibcode = 2009ApJ...706L.230M |doi = 10.1088/0004-637X/706/2/L230 |year=2009|s2cid=17750440}}</ref> || 20:24:04 +33:52:03
|-
|-
|[[GX 339-4]]/[[V821 Ara]] ||5.8 || 5–6 || 1.75 || 15,000 || 17:02:50 -48:47:23
|[[4U 1543-475]]/IL Lupi || 9.4&nbsp;±&nbsp;1.0 || 0.25 || 1.1 || 24000 || 15:47:09 −47:40:10
|-
|-
|[[Gaia BH2]]
|[[GRS 1124-683]]/[[GU Mus]] || 7.0 ± 0.6 || || 0.43 || 17,000 || 11:26:27 -68:40:32
|8.94&nbsp;±&nbsp;0.34
|1.07&nbsp;±&nbsp;0.19
|1,276.7&nbsp;±&nbsp;0.6
|{{0}}3800
|13:50:17 −59:14:20
|-
|-
|[[MAXI J1305-704]]<ref>{{Cite journal |last1=Mata Sánchez |first1=D. |last2=Rau |first2=A. |last3=Álvarez Hernández |first3=A. |last4=van Grunsven |first4=T. F. J. |last5=Torres |first5=M. A. P. |last6=Jonker |first6=P. G. |date=2021-09-01 |title=Dynamical confirmation of a stellar mass black hole in the transient X-ray dipping binary MAXI J1305-704 |journal=Monthly Notices of the Royal Astronomical Society |volume=506 |issue=1 |pages=581–594 |doi=10.1093/mnras/stab1714 |doi-access=free |arxiv=2104.07042 |bibcode=2021MNRAS.506..581M |issn=0035-8711}}</ref>
|[[XTE J1550-564]]/[[V381 Nor]] || 9.6 ± 1.2 || 6.0–7.5 || 1.5 || 17,000 ||15:50:59 -56:28:36
|{{Val|8.9|1.6|1.0}}
|0.43&nbsp;±&nbsp;0.16
|0.394&nbsp;±&nbsp;0.004
|24500
|13:06:55 −70:27:05
|-
|-
|[[BW Circini|GS 1354-64 (BW Cir)]]<ref>{{Cite journal |last1=Casares |first1=J. |last2=Orosz |first2=J. A. |last3=Zurita |first3=C. |last4=Shahbaz |first4=T. |last5=Corral-Santana |first5=J. M. |last6=McClintock |first6=J. E. |last7=Garcia |first7=M. R. |last8=Martínez-Pais |first8=I. G. |last9=Charles |first9=P. A. |last10=Fender |first10=R. P. |last11=Remillard |first11=R. A. |date=2009-03-01 |title=Refined Orbital Solution and Quiescent Variability in the Black Hole Transient GS 1354-64 (= BW Cir) |url=https://ui.adsabs.harvard.edu/abs/2009ApJS..181..238C |journal=The Astrophysical Journal Supplement Series |volume=181 |issue=1 |pages=238–243 |doi=10.1088/0067-0049/181/1/238 |bibcode=2009ApJS..181..238C |issn=0067-0049|hdl=1721.1/95899 |hdl-access=free }}</ref>
|[[4U 1543-475]]/[[IL Lupi]] || 9.4 ± 1.0 || 0.25 || 1.1 || 24,000 || 15:47:09 -47:40:10
|7.9&nbsp;±&nbsp;0.5
|1.1&nbsp;±&nbsp;0.1
|2.5445
|>81500
|13:58:10 −64:44:06
|-
|-
|[[XTE J1859+226|XTE J1859+226 (V406 Vul)]]<ref>{{Cite journal |last1=Yanes-Rizo |first1=I. V. |last2=Torres |first2=M. A. P. |last3=Casares |first3=J. |last4=Motta |first4=S. E. |last5=Muñoz-Darias |first5=T. |last6=Rodríguez-Gil |first6=P. |last7=Armas Padilla |first7=M. |last8=Jiménez-Ibarra |first8=F. |last9=Jonker |first9=P. G. |last10=Corral-Santana |first10=J. M. |last11=Fender |first11=R. |date=2022-11-01 |title=A refined dynamical mass for the black hole in the X-ray transient XTE J1859+226 |journal=Monthly Notices of the Royal Astronomical Society |volume=517 |issue=1 |pages=1476–1482 |doi=10.1093/mnras/stac2719 |doi-access=free |arxiv=2209.10395 |bibcode=2022MNRAS.517.1476Y |issn=0035-8711}}</ref>
|[[XTE J1819-254]]/[[V4641 Sgr]] || 7.1 ± 0.3 || 5–8 || 2.82 || 24,000–40,000<ref>{{cite journal |last=Orosz |display-authors=etal |title=A Black Hole in the Superluminal source SAX J1819.3-2525 (V4641 Sgr) |journal=The Astrophysical Journal |year=2001 |volume=555 |issue=1 |pages=489 |doi=10.1086/321442 |arxiv=astro-ph/0103045v1 |bibcode=2001ApJ...555..489O |s2cid=50248739 }}</ref>|| 18:19:22 -25:24:25
|7.8&nbsp;±&nbsp;1.9
|0.55&nbsp;±&nbsp;0.16
|0.276&nbsp;±&nbsp;0.003
|
|18:58:42 +22:39:29
|-
|[[HD 130298]]<ref>{{Cite journal |last1=Mahy |first1=L. |last2=Sana |first2=H. |last3=Shenar |first3=T. |last4=Sen |first4=K. |last5=Langer |first5=N. |last6=Marchant |first6=P. |last7=Abdul-Masih |first7=M. |last8=Banyard |first8=G. |last9=Bodensteiner |first9=J. |last10=Bowman |first10=D. M. |last11=Dsilva |first11=K. |last12=Fabry |first12=M. |last13=Hawcroft |first13=C. |last14=Janssens |first14=S. |last15=Van Reeth |first15=T. |date=2022-08-01 |title=Identifying quiescent compact objects in massive Galactic single-lined spectroscopic binaries |url=https://ui.adsabs.harvard.edu/abs/2022A&A...664A.159M |journal=Astronomy and Astrophysics |volume=664 |pages=A159 |doi=10.1051/0004-6361/202243147 |arxiv=2207.07752 |bibcode=2022A&A...664A.159M |issn=0004-6361}}</ref>
|>7.7&nbsp;±&nbsp;1.5
|24.2&nbsp;±&nbsp;3.8
|14.60
|{{0}}7910
|14:49:34 −56:25:38
|-
|[[NGC 3201 21859|NGC 3201 #21859]]<ref name=":1">{{Cite journal |last1=Giesers |first1=Benjamin |last2=Kamann |first2=Sebastian |last3=Dreizler |first3=Stefan |last4=Husser |first4=Tim-Oliver |last5=Askar |first5=Abbas |last6=Göttgens |first6=Fabian |last7=Brinchmann |first7=Jarle |last8=Latour |first8=Marilyn |last9=Weilbacher |first9=Peter M. |last10=Wendt |first10=Martin |last11=Roth |first11=Martin M. |date=2019-12-01 |title=A stellar census in globular clusters with MUSE: Binaries in NGC 3201 |url=https://ui.adsabs.harvard.edu/abs/2019A&A...632A...3G |journal=Astronomy and Astrophysics |volume=632 |pages=A3 |doi=10.1051/0004-6361/201936203 |arxiv=1909.04050 |bibcode=2019A&A...632A...3G |issn=0004-6361}}</ref><ref name=":2">{{Cite journal |last=Rodriguez |first=Carl L. |date=2023-04-01 |title=Constraints on the Cosmological Coupling of Black Holes from the Globular Cluster NGC 3201 |journal=The Astrophysical Journal |volume=947 |issue=1 |pages=L12 |doi=10.3847/2041-8213/acc9b6 |doi-access=free |arxiv=2302.12386 |bibcode=2023ApJ...947L..12R |issn=0004-637X}}</ref>
|7.68&nbsp;±&nbsp;0.50
|0.61&nbsp;±&nbsp;0.05
|2.2422&nbsp;±&nbsp;0.0001
|15700
|10:17:39 −46:24:25
|-
|[[GS 2000+25]]/QZ Vul || 7.5&nbsp;±&nbsp;0.3 || 4.9...5.1 || 0.35 || {{0}}8800 || 20:02:50 +25:14:11
|-
|[[V4641 Sagittarii|XTE J1819-254]]/V4641 Sgr || 7.1&nbsp;±&nbsp;0.3 || 5...8 || 2.82 || 24000...40000<ref>{{cite journal |last=Orosz |display-authors=etal |title=A Black Hole in the Superluminal source SAX J1819.3-2525 (V4641 Sgr) |journal=The Astrophysical Journal |year=2001 |volume=555 |issue=1 |pages=489 |doi=10.1086/321442 |arxiv=astro-ph/0103045v1 |bibcode=2001ApJ...555..489O |s2cid=50248739 }}</ref>|| 18:19:22 −25:24:25
|-
|[[LB-1]] (disputed)<ref name="Shenar_etal_2020">{{cite journal |author1=Shenar, T. |author2=Bodensteiner, J. |author3=Abdul-Masih, M. |author4=Fabry, M. |author5=Marchant, P. |author6=Banyard, G. |author7=Bowman, D. M. |author8=Dsilva, K. |author9=Hawcroft, C. |author10=Reggiani, M. |author11=Sana, H. |date=July 2020 |title=The 'hidden' companion in LB-1 unveiled by spectral disentangling |journal=Astronomy and Astrophysics |type=Letter to the Editor |volume=630 |pages=L6 |arxiv=2004.12882 |bibcode=2020A&A...639L...6S |doi=10.1051/0004-6361/202038275 |doi-access=free}}</ref> || 7&nbsp;±&nbsp;2<ref name="Shenar_etal_2020" /> || 1.5&nbsp;±&nbsp;0.4<ref name="Shenar_etal_2020" /> || 78.7999&nbsp;±&nbsp;0.0097<ref name="Shenar_etal_2020" /> ||15000<ref name="EA-20191127a">{{cite web |author=Chinese Academy of Science |author-link=Chinese Academy of Science |date=27 November 2019 |title=Chinese Academy of Sciences leads discovery of unpredicted stellar black hole |url=https://www.eurekalert.org/pub_releases/2019-11/caos-cao112519.php |url-status=live |archive-url=https://web.archive.org/web/20191128233834/https://www.eurekalert.org/pub_releases/2019-11/caos-cao112519.php |archive-date=28 November 2019 |access-date=29 November 2019 |work=[[EurekAlert!]]}}</ref> || 06:11:49&nbsp;+22:49:32<ref name="NAT-20191127">{{cite journal |author=Liu, Jifeng |display-authors=et al. |date=27 November 2019 |title=A wide star–black-hole binary system from radial-velocity measurements |journal=[[Nature (journal)|Nature]] |volume=575 |issue=7784 |pages=618–621 |arxiv=1911.11989 |bibcode=2019Natur.575..618L |doi=10.1038/s41586-019-1766-2 |pmid=31776491 |s2cid=208310287}}</ref>
|-
|[[GRS 1124-683]]/Nova Muscae 1991/GU Mus
| 7.0&nbsp;±&nbsp;0.6 || || 0.43 || 17000 || 11:26:27 −68:40:32
|-
|[[H 1705-25]]/Nova Ophiuchi 1977/V2107 Oph<ref>{{Cite journal |last1=Dashwood Brown |first1=Cordelia |last2=Gandhi |first2=Poshak |last3=Zhao |first3=Yue |date=2024-01-01 |title=On the natal kick of the black hole X-ray binary H 1705-250 |journal=Monthly Notices of the Royal Astronomical Society |volume=527 |issue=1 |pages=L82–L87 |doi=10.1093/mnrasl/slad151 |doi-access=free |arxiv=2310.11492 |bibcode=2024MNRAS.527L..82D |issn=0035-8711}}</ref>
|6.95&nbsp;±&nbsp;1.35<ref>{{Cite journal |last1=Remillard |first1=Ronald A. |last2=McClintock |first2=Jeffrey E. |date=2006-09-01 |title=X-Ray Properties of Black-Hole Binaries |url=https://ui.adsabs.harvard.edu/abs/2006ARA&A..44...49R |journal=Annual Review of Astronomy and Astrophysics |volume=44 |issue=1 |pages=49–92 |doi=10.1146/annurev.astro.44.051905.092532 |arxiv=astro-ph/0606352 |bibcode=2006ARA&A..44...49R |issn=0066-4146}}</ref>
|0.34&nbsp;±&nbsp;0.08
|0.52125
|
|17:08:15 −25:05:30
|-
|[[XTE J1118+480]]/KV UMa || 6.8&nbsp;±&nbsp;0.4 || 6...6.5 || 0.17 || {{0}}6200 || 11:18:11 +48:02:13
|-
|[[MAXI J1820+070]]<ref>{{Cite journal |last1=Mikołajewska |first1=Joanna |last2=Zdziarski |first2=Andrzej A. |last3=Ziółkowski |first3=Janusz |last4=Torres |first4=Manuel A. P. |last5=Casares |first5=Jorge |date=2022-05-01 |title=The Donor of the Black Hole X-Ray Binary MAXI J1820+070 |journal=The Astrophysical Journal |volume=930 |issue=1 |pages=9 |doi=10.3847/1538-4357/ac6099 |doi-access=free |arxiv=2201.13201 |bibcode=2022ApJ...930....9M |issn=0004-637X}}</ref>
|{{Val|6.75|0.64|0.46}}
|0.49&nbsp;±&nbsp;0.1
|0.68549&nbsp;±&nbsp;0.00001
|{{0}}9800
|18:20:22 +07:11:07
|-
|[[GRO J1655-40]]/V1033 Sco || 6.3&nbsp;±&nbsp;0.3 || 2.6...2.8 || 2.8 || {{0}}5000...11000|| 16:54:00 −39:50:45
|-
|[[GX 339-4]]/V821 Ara ||5.8 || 5...6 || 1.75 || 15000 || 17:02:50 −48:47:23
|-
|[[GRO J1719-24]]|| {{sort|5|≥4.9}}|| ≈1.6 || possibly 0.6<ref name="Masetti1996">{{citation|
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 }}</ref>|| {{0}}8500 || 17:19:37 −25:01:03
|-
|[[NGC 3201 12560|NGC 3201 #12560]]<ref name=":1" /><ref name=":2" />
|4.53&nbsp;±&nbsp;0.21
|0.81&nbsp;±&nbsp;0.05
|167.01&nbsp;±&nbsp;0.09
|15700
|10:17:37 −46:24:55
|-
|-
|[[GRS 1009-45]]&nbsp;/<br>Nova Velorum 1993/MM Velorum<ref>{{Cite journal |last1=Filippenko |first1=Alexei V. |last2=Leonard |first2=Douglas C. |last3=Matheson |first3=Thomas |last4=Li |first4=Weidong |last5=Moran |first5=Edward C. |last6=Riess |first6=Adam G. |date=1999-08-01 |title=A Black Hole in the X-Ray Nova Velorum 1993 |url=https://ui.adsabs.harvard.edu/abs/1999PASP..111..969F |journal=Publications of the Astronomical Society of the Pacific |volume=111 |issue=762 |pages=969–979 |doi=10.1086/316413 |arxiv=astro-ph/9904271 |bibcode=1999PASP..111..969F |issn=0004-6280}}</ref>
|[[GRS 1915+105]]/[[V1487 Aql]] || 14 ± 4.0 || ~1 || 33.5 || 40,000 ||19:15:12 +10:56:44
|4.3&nbsp;±&nbsp;0.1
|0.5...0.65
|0.285206&nbsp;±<br>0.0000014
|17200
|10:13:36 −45:04:33
|-
|-
|[[GRO J0422+32]]/V518 Per|| 4&nbsp;±&nbsp;1 || 1.1 || 0.21 || {{0}}8500 || 04:21:43 +32:54:27
|[[XTE J1650-500]] || 9.7 ± 1.6<ref>{{cite journal |title=Determination of Black Hole Masses in Galactic Black Hole Binaries using Scaling of Spectral and Variability Characteristics |last1=Shaposhnikov |first1=N. |last2=Titarchuk |first2=L. |date=2009 |journal=The Astrophysical Journal |volume=699 |issue=1 |pages=453–468 |doi=10.1088/0004-637X/699/1/453 |arxiv=0902.2852v1 |bibcode=2009ApJ...699..453S |s2cid=18336866 }}</ref> || 5–10 || 0.32<ref>{{cite journal |title=Orbital Parameters for the Black Hole Binary XTE J1650–500 |display-authors=1 |last1=Orosz |first1=J.A. |last2=McClintock |first2=J.E. |last3=Remillard |first3=R.A. |last4=Corbel |first4=S. |date=2004 |journal=The Astrophysical Journal |volume=616 |issue=1 |pages=376–382 |bibcode=2004ApJ...616..376O |doi=10.1086/424892 |arxiv=astro-ph/0404343 |s2cid=13933140 }}</ref> || 10,763||16:50:01 -49:57:45
|}
|}


Line 109: Line 201:
!Name || [[Black hole|BHC]] mass<br />([[solar mass]]es)|| Companion mass<br />(solar masses ) || [[Orbital period]]<br />(days) || Distance from Earth<br />([[light year]]s) || Location<ref name="ReferenceA"/>
!Name || [[Black hole|BHC]] mass<br />([[solar mass]]es)|| Companion mass<br />(solar masses ) || [[Orbital period]]<br />(days) || Distance from Earth<br />([[light year]]s) || Location<ref name="ReferenceA"/>
|-
|-
|[[GW150914]] (62 ± 4) {{Solar mass}} || 36 ± 4 || 29 ± 4 || .|| 1.3&nbsp;billion ||
|[[GW190521]] ({{Val|155|17|11}}) {{Solar mass}}
|{{Val|78|9|5}}<ref name="Gayathri+2020">{{cite arXiv |eprint=2009.05461 |class=astro-ph.HE |author=Gayathri, V. |title=GW190521 as a Highly Eccentric Black Hole Merger |display-authors=et al. |year=2020}}</ref>
|{{Val|78|9|5}}<ref name="Gayathri+2020" />
|
|
|
|-
|-
|[[GW170104]] (48.7 ± 5) {{Solar mass}}
|[[GW150914]] (62&nbsp;±&nbsp;4) {{Solar mass}} || 36&nbsp;±&nbsp;4 || 29&nbsp;±&nbsp;4 || . || 1.3&nbsp;billion ||
|-
|31.2 ± 7
|[[GW170104]] (48.7&nbsp;±&nbsp;5) {{Solar mass}}
|19.4 ± 6
|31.2&nbsp;±&nbsp;7
|.
|19.4&nbsp;±&nbsp;6
| .
|1.4&nbsp;billion
|1.4&nbsp;billion
|
|
|-
|-
|[[GW151226]] (21.8 ± 3.5) {{Solar mass}}
|[[GW170814]] ({{Val|53.2|3.2|2.5}}) {{Solar mass}}
|{{Val|30.5|5.7|3.0}}
|14.2 ± 6
|{{Val|25.3|2.8|4.2}}
|7.5 ± 2.3
|
|1.8&nbsp;billion
|
|-
|[[GW190412]]
|29.7
|8.4
|
|2.4&nbsp;billion
|
|-
|[[GW190814]]
|22.2–24.3
|2.50–2.67
|
|
|
|-
|[[GW151226]] (21.8&nbsp;±&nbsp;3.5) {{Solar mass}}
|14.2&nbsp;±&nbsp;6
|7.5&nbsp;±&nbsp;2.3
|.
|.
|2.9&nbsp;billion
|2.9&nbsp;billion
|
|
|-
|[[GW170608]]
|{{Val|12|7|2}}
|7&nbsp;±&nbsp;2
|
|1.1&nbsp;billion
|
|}

Candidates outside our galaxy from X-ray binaries:
{| class="wikitable sortable"
!Name
!Host galaxy|| [[Black hole|BHC]] mass<br />([[solar mass]]es)|| Companion mass<br />(solar masses ) || [[Orbital period]]<br />(days) || Distance from Earth<br />([[light year]]s)
|-
|[[IC 10 X-1]]<ref>{{Cite journal |last1=Laycock |first1=Silas G. T. |last2=Cappallo |first2=Rigel C. |last3=Moro |first3=Matthew J. |date=2015-01-01 |title=Chandra and XMM monitoring of the black hole X-ray binary IC 10 X-1 |journal=Monthly Notices of the Royal Astronomical Society |volume=446 |issue=2 |pages=1399–1410 |doi=10.1093/mnras/stu2151 |doi-access=free |arxiv=1410.3417 |bibcode=2015MNRAS.446.1399L |issn=0035-8711}}</ref>
|[[IC 10]]
|≥23.1&nbsp;±&nbsp;2.1
|≥17
|1.45175
|2.15&nbsp;million
|-
|[[NGC 300 X-1]]<ref>{{Cite journal |last1=Binder |first1=Breanna A. |last2=Sy |first2=Janelle M. |last3=Eracleous |first3=Michael |last4=Christodoulou |first4=Dimitris M. |last5=Bhattacharya |first5=Sayantan |last6=Cappallo |first6=Rigel |last7=Laycock |first7=Silas |last8=Plucinsky |first8=Paul P. |last9=Williams |first9=Benjamin F. |date=2021-03-01 |title=The Wolf-Rayet + Black Hole Binary NGC 300 X-1: What is the Mass of the Black Hole? |journal=The Astrophysical Journal |volume=910 |issue=1 |pages=74 |doi=10.3847/1538-4357/abe6a9 |doi-access=free |arxiv=2102.07065 |bibcode=2021ApJ...910...74B |issn=0004-637X}}</ref>
|[[NGC 300]]
|17&nbsp;±&nbsp;4
|{{Val|26|7|5}}
|1.3663375
|6.5&nbsp;million
|-
|[[M33 X-7]]
|[[Triangulum Galaxy]]
|15.65&nbsp;±&nbsp;1.45
|70&nbsp;±&nbsp;6.9
|3.45301&nbsp;±&nbsp;0.00002
|2.7&nbsp;million
|-
|[[LMC X-1]]<ref>{{Cite journal |last1=Orosz |first1=Jerome A. |last2=Steeghs |first2=Danny |last3=McClintock |first3=Jeffrey E. |last4=Torres |first4=Manuel A. P. |last5=Bochkov |first5=Ivan |last6=Gou |first6=Lijun |last7=Narayan |first7=Ramesh |last8=Blaschak |first8=Michael |last9=Levine |first9=Alan M. |last10=Remillard |first10=Ronald A. |last11=Bailyn |first11=Charles D. |last12=Dwyer |first12=Morgan M. |last13=Buxton |first13=Michelle |date=2009-05-01 |title=A New Dynamical Model for the Black Hole Binary LMC X-1 |url=https://ui.adsabs.harvard.edu/abs/2009ApJ...697..573O |journal=The Astrophysical Journal |volume=697 |issue=1 |pages=573–591 |doi=10.1088/0004-637X/697/1/573 |arxiv=0810.3447 |bibcode=2009ApJ...697..573O |issn=0004-637X}}</ref>
|[[Large Magellanic Cloud]]
|10.91&nbsp;±&nbsp;1.41
|31.79&nbsp;±&nbsp;3.48
|3.9094&nbsp;±&nbsp;0.0008
|180,000<ref>{{Cite journal |last1=Haardt |first1=F. |last2=Galli |first2=M. R. |last3=Treves |first3=A. |last4=Chiappetti |first4=L. |last5=Dal Fiume |first5=D. |last6=Corongiu |first6=A. |last7=Belloni |first7=T. |last8=Frontera |first8=F. |last9=Kuulkers |first9=E. |last10=Stella |first10=L. |date=2001-03-01 |title=Broadband X-Ray Spectra of the Persistent Black Hole Candidates LMC X-1 and LMC X-3 |url=https://ui.adsabs.harvard.edu/abs/2001ApJS..133..187H |journal=The Astrophysical Journal Supplement Series |volume=133 |issue=1 |pages=187–193 |doi=10.1086/319186 |arxiv=astro-ph/0009231 |bibcode=2001ApJS..133..187H |issn=0067-0049}}</ref>
|-
|[[LMC X-3]]<ref>{{Cite journal |last1=Orosz |first1=Jerome A. |last2=Steiner |first2=James F. |last3=McClintock |first3=Jeffrey E. |last4=Buxton |first4=Michelle M. |last5=Bailyn |first5=Charles D. |last6=Steeghs |first6=Danny |last7=Guberman |first7=Alec |last8=Torres |first8=Manuel A. P. |date=2014-10-01 |title=The Mass of the Black Hole in LMC X-3 |url=https://ui.adsabs.harvard.edu/abs/2014ApJ...794..154O |journal=The Astrophysical Journal |volume=794 |issue=2 |pages=154 |doi=10.1088/0004-637X/794/2/154 |arxiv=1402.0085 |bibcode=2014ApJ...794..154O |issn=0004-637X}}</ref>
|Large Magellanic Cloud
|6.98&nbsp;±&nbsp;0.56
|3.63&nbsp;±&nbsp;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.<ref name=adams>{{cite arXiv|last1=Adams|first1=S. M.|last2=Kochanek|first2=C. S|last3=Gerke|first3=J. R.|last4=Stanek|first4=K. Z.|last5=Dai|first5=X.|title=The search for failed supernovae with the Large Binocular Telescope: conformation of a disappearing star|date=9 September 2016|eprint=1609.01283v1|class=astro-ph.SR}}</ref>
The disappearance of [[N6946-BH1]] following a [[failed supernova]] in [[NGC 6946]] may have resulted in the formation of a black hole.<ref name="adams">{{cite arXiv|last1=Adams|first1=S. M.|last2=Kochanek|first2=C. S|last3=Gerke|first3=J. R.|last4=Stanek|first4=K. Z.|last5=Dai|first5=X.|title=The search for failed supernovae with the Large Binocular Telescope: conformation of a disappearing star|date=9 September 2016|eprint=1609.01283v1|class=astro-ph.SR}}</ref>


==See also==
==See also==
Line 132: Line 300:
* [[Supermassive black hole]]
* [[Supermassive black hole]]
* [[Rogue black hole]]
* [[Rogue black hole]]
* [[Primordial black hole]]


==References==
==References==

Latest revision as of 23:14, 29 October 2024

Not to be confused with black hole star.

Artist's impression of a stellar-mass black hole (left) in the spiral galaxy NGC 300; it is associated with a Wolf–Rayet star

A stellar black hole (or stellar-mass black hole) is a black hole formed by the gravitational collapse of a star.[1] They have masses ranging from about 5 to several tens of solar masses.[2] 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

[edit]

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.[3] The maximum observed mass of neutron stars is about 2.14 M☉ for PSR J0740+6620 discovered in September, 2019.[4]

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 15.65±1.45 solar masses.[5] In September 2015, a rotating black hole of 62±4 solar masses was discovered by gravitational waves as it formed in a merger event of two smaller black holes.[6] As of June 2020, the binary system 2MASS J05215658+4359220 was reported[7] 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

[edit]

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

[edit]

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,[8] which may be due to the fall-back of asymmetrically expelled matter increasing the momentum of the resulting black hole.[9]

Mass gaps

[edit]

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 (M☉), respectively.[10] Another range given for the upper gap is 52 to 133 M☉.[11] 150 M☉ has been regarded as the upper mass limit for stars in the current era of the universe.[12]

Lower mass gap

[edit]

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.[10] The existence and theoretical basis for this possible gap are uncertain.[13] 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.[14] 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 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.[15]

Upper mass gap

[edit]

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.[16] 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.[17]

Pair-instability supernovae can only happen in stars with a mass range from around 130 to 250 solar masses (M☉) 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.[18] In nonrotating stars the lower bound of the upper mass gap may be as high as 60 M☉.[19] The possibility of direct collapse into black holes of stars with core mass > 133 M☉, requiring total stellar mass of > 260 M☉ 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.[11]

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

[edit]
See also: List of black holes and 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.[20][21][22]

Name Mass (solar masses) Orbital period
(days) 		Distance
from
Earth (ly) 		Celestial
Coordinates[23]
BHC Companion
Gaia BH3 32.70 ± 0.82 0.76 ± 0.05 4,253.1 ± 98.5 1926 19:39:19 +14:55:54
Cyg X-1 21.2 ± 2.2[24] 40.6+7.7
−7.1[24]		 5.6 6000...8000 19:58:22 +35:12:06
GRS 1915+105/V1487 Aql 14 ± 4.0 ≈1 33.5 40000 19:15:12 +10:56:44
V404 Cyg 12 ± 2 6.0 6.5 7800 ± 460[25] 20:24:04 +33:52:03
A0620-00/V616 Mon 11 ± 2 2.6–2.8 0.33 3500 06:22:44 −00:20:45
XTE J1650-500 9.7 ± 1.6[26] 5–10 0.32[27] 10763 16:50:01 −49:57:45
Gaia BH1 9.62 ± 0.18 0.93 ± 0.05 185.59 ± 0.05 1560 17:28:41 −00:34:52
XTE J1550-564/V381 Nor 9.6 ± 1.2 6.0...7.5 1.5 17000 15:50:59 −56:28:36
4U 1543-475/IL Lupi 9.4 ± 1.0 0.25 1.1 24000 15:47:09 −47:40:10
Gaia BH2 8.94 ± 0.34 1.07 ± 0.19 1,276.7 ± 0.6 3800 13:50:17 −59:14:20
MAXI J1305-704[28] 8.9+1.6
−1.0 		0.43 ± 0.16 0.394 ± 0.004 24500 13:06:55 −70:27:05
GS 1354-64 (BW Cir)[29] 7.9 ± 0.5 1.1 ± 0.1 2.5445 >81500 13:58:10 −64:44:06
XTE J1859+226 (V406 Vul)[30] 7.8 ± 1.9 0.55 ± 0.16 0.276 ± 0.003 18:58:42 +22:39:29
HD 130298[31] >7.7 ± 1.5 24.2 ± 3.8 14.60 7910 14:49:34 −56:25:38
NGC 3201 #21859[32][33] 7.68 ± 0.50 0.61 ± 0.05 2.2422 ± 0.0001 15700 10:17:39 −46:24:25
GS 2000+25/QZ Vul 7.5 ± 0.3 4.9...5.1 0.35 8800 20:02:50 +25:14:11
XTE J1819-254/V4641 Sgr 7.1 ± 0.3 5...8 2.82 24000...40000[34] 18:19:22 −25:24:25
LB-1 (disputed)[35] 7 ± 2[35] 1.5 ± 0.4[35] 78.7999 ± 0.0097[35] 15000[36] 06:11:49 +22:49:32[37]
GRS 1124-683/Nova Muscae 1991/GU Mus 7.0 ± 0.6 0.43 17000 11:26:27 −68:40:32
H 1705-25/Nova Ophiuchi 1977/V2107 Oph[38] 6.95 ± 1.35[39] 0.34 ± 0.08 0.52125 17:08:15 −25:05:30
XTE J1118+480/KV UMa 6.8 ± 0.4 6...6.5 0.17 6200 11:18:11 +48:02:13
MAXI J1820+070[40] 6.75+0.64
−0.46 		0.49 ± 0.1 0.68549 ± 0.00001 9800 18:20:22 +07:11:07
GRO J1655-40/V1033 Sco 6.3 ± 0.3 2.6...2.8 2.8 5000...11000 16:54:00 −39:50:45
GX 339-4/V821 Ara 5.8 5...6 1.75 15000 17:02:50 −48:47:23
GRO J1719-24 ≥4.9 ≈1.6 possibly 0.6[41] 8500 17:19:37 −25:01:03
NGC 3201 #12560[32][33] 4.53 ± 0.21 0.81 ± 0.05 167.01 ± 0.09 15700 10:17:37 −46:24:55
GRS 1009-45 /
Nova Velorum 1993/MM Velorum[42] 		4.3 ± 0.1 0.5...0.65 0.285206 ±
0.0000014 		17200 10:13:36 −45:04:33
GRO J0422+32/V518 Per 4 ± 1 1.1 0.21 8500 04:21:43 +32:54:27

Extragalactic

[edit]

Candidates outside our galaxy come from gravitational wave detections:

Outside our galaxy
Name BHC mass
(solar masses)		 Companion mass
(solar masses )		 Orbital period
(days)		 Distance from Earth
(light years)		 Location[23]
GW190521 (155+17
−11) M☉ 		78+9
−5[43] 		78+9
−5[43]
GW150914 (62 ± 4) M☉ 36 ± 4 29 ± 4 . 1.3 billion
GW170104 (48.7 ± 5) M☉ 31.2 ± 7 19.4 ± 6 . 1.4 billion
GW170814 (53.2+3.2
−2.5) M☉ 		30.5+5.7
−3.0 		25.3+2.8
−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 ± 3.5) M☉ 14.2 ± 6 7.5 ± 2.3 . 2.9 billion
GW170608 12+7
−2 		7 ± 2 1.1 billion

Candidates outside our galaxy from X-ray binaries:

Name Host galaxy BHC mass
(solar masses)		 Companion mass
(solar masses )		 Orbital period
(days)		 Distance from Earth
(light years)
IC 10 X-1[44] IC 10 ≥23.1 ± 2.1 ≥17 1.45175 2.15 million
NGC 300 X-1[45] NGC 300 17 ± 4 26+7
−5 		1.3663375 6.5 million
M33 X-7 Triangulum Galaxy 15.65 ± 1.45 70 ± 6.9 3.45301 ± 0.00002 2.7 million
LMC X-1[46] Large Magellanic Cloud 10.91 ± 1.41 31.79 ± 3.48 3.9094 ± 0.0008 180,000[47]
LMC X-3[48] Large Magellanic Cloud 6.98 ± 0.56 3.63 ± 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.[49]

See also

[edit]

References

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