101:
1783:
31:
426:
1793:
108:
X-ray binaries are further subdivided into several (sometimes overlapping) subclasses, that perhaps reflect the underlying physics better. Note that the classification by mass (high, intermediate, low) refers to the optically visible donor, not to the compact X-ray emitting accretor.
358:
In a high-mass X-ray binary, the massive star dominates the emission of optical light, while the compact object is the dominant source of X-rays. The massive stars are very luminous and therefore easily detected. One of the most famous high-mass X-ray binaries is
488:. The jets are formed close to the compact object, and timescales near the compact object are proportional to the mass of the compact object. Therefore, ordinary quasars take centuries to go through variations a microquasar experiences in one day.
80:
releases only about 0.7 percent of rest mass.) The lifetime and the mass-transfer rate in an X-ray binary depends on the evolutionary status of the donor star, the mass ratio between the stellar components, and their orbital separation.
307:) is a binary star system where one of the components is a neutron star or a black hole. The other component is an intermediate-mass star. An intermediate-mass X-ray binary is the origin for Low-mass X-ray binary systems.
465:); in microquasars, the mass of the compact object is only a few solar masses. In microquasars, the accreted mass comes from a normal star, and the accretion disk is very luminous in the optical and
1053:
Tauris, Thomas M; Van Den Heuvel, Edward P. J; Savonije, Gerrit J (2000). "Formation of
Millisecond Pulsars with Heavy White Dwarf Companions:Extreme Mass Transfer on Subthermal Timescales".
1692:
870:
Negueruela, I; Smith, D. M; Reig, P; Chaty, S; TorrejĂłn, J. M (2006). "Supergiant Fast X-ray
Transients: A New Class of High Mass X-ray Binaries Unveiled by INTEGRAL".
445:. Microquasars are named after quasars, as they have some common characteristics: strong and variable radio emission, often resolvable as a pair of radio jets, and an
563:
Tauris, Thomas M.; van den Heuvel, Ed (2006). "Chapter 16: Formation and evolution of compact stellar X-ray sources". In Lewin, Walter; van der Klis, Michiel (eds.).
264:, and typically less than one percent in visible light, so they are among the brightest objects in the X-ray sky, but relatively faint in visible light. The
1532:
507:(E > 60 MeV). Extremely high energies of particles emitting in the VHE band might be explained by several mechanisms of particle acceleration (see
944:
Liu, Q. Z; Van
Paradijs, J; Van Den Heuvel, E. P. J (2007). "A catalogue of low-mass X-ray binaries in the Galaxy, LMC, and SMC (Fourth edition)".
1317:
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overflow of the massive normal star accretes in such large quantities, the transfer is very unstable and creates a short lived mass transfer.
1756:
761:
598:
512:
1832:
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and therefore transfers mass to the compact star. In LMXB systems the donor is less massive than the compact object, and can be on the
1766:
1232:. A Population Explosion: The Nature & Evolution of X-Ray Binaries in Diverse Environments. Vol. 1010. pp. 252–256.
1715:
1827:
1117:
Podsiadlowski, Ph; Rappaport, S; Pfahl, E. D (2002). "Evolutionary
Sequences for Low- and Intermediate-Mass X-Ray Binaries".
813:"Evolution of Intermediate-mass X-Ray Binaries Driven by the Magnetic Braking of AP/BP Stars. I. Ultracompact X-Ray Binaries"
1741:
1720:
1661:
402:
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622:
Weidenspointner, Georg (2008). "An asymmetric distribution of positrons in the
Galactic disk revealed by gamma-rays".
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250:
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Once a HMXB has reached its end, if the periodicity of the binary was less than a year, it can become a single
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288:
130:
125:
1837:
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1371:
722:
Patruno, Alessandro; Watts, Anna L. (2021), Belloni, Tomaso M.; MĂ©ndez, Mariano; Zhang, Chengmin (eds.),
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are due to the accretion of matter magnetically funneled into the poles of the compact companion. The
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around the compact object. The orbital periods of LMXBs range from ten minutes to hundreds of days.
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Negueruela, Ignacio; Torrejon, Jose Miguel; Reig, Pablo; Ribo, Marc; Smith, David M. (2008).
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Tetarenko, B. E.; Sivakoff, G. R.; Heinke, C. O.; Gladstone, J. C. (February 10, 2010).
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system that is strong in X rays, and in which the normal stellar component is a massive
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to distinguish them from other X-ray binaries. A part of the radio emission comes from
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999:"Watchdog: A Comprehensive All-Sky Database of Galactic Black Hole X-Ray Binaries"
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685:
194:(radio-jet X-ray binaries that can house either a neutron star or a black hole)
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409:. With a longer periodicity, a year and beyond, the HMXB can become a double
363:, which was the first identified black hole candidate. Other HMXBs include
1597:
1580:
414:
242:
238:
49:. The X-rays are produced by matter falling from one component, called the
30:
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651:
425:
351:
of the massive normal star is captured by the compact object, and produces
1602:
1361:
1131:
1067:
907:
Sidoli, Lara; Ed van den Heuvel (2008). "Transient outburst mechanisms".
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573:
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is typically around 15 to 20. The brightest part of the system is the
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730:, vol. 461, Berlin, Heidelberg: Springer, pp. 143–208,
567:. Cambridge Astrophysics Series. Vol. 39. pp. 623–665.
328:
57:
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1295:
728:
Timing
Neutron Stars: Pulsations, Oscillations and Explosions
495:, in which atomic emission lines are visible from both jets;
241:). Approximately two hundred LMXBs have been detected in the
441:(or radio emitting X-ray binary) is the smaller cousin of a
499:, with an especially high jet velocity and the very bright
76:, up to 30 percent of its rest mass, as X-rays. (Hydrogen
461:. In quasars, the black hole is supermassive (millions of
1230:
Supergiant Fast X-ray
Transients and Other Wind Accretors
256:
A typical low-mass X-ray binary emits almost all of its
1693:
Timeline of white dwarfs, neutron stars, and supernovae
275:
The variability of LMXBs are most commonly observed as
245:, and of these, thirteen LMXBs have been discovered in
378:
The variability of HMXBs are observed in the form of
1734:
1701:
1675:
1546:
1448:
1390:
1354:
1333:
225:. The other component, a donor, usually fills its
141:
484:Microquasars are very important for the study of
291:created by the accretion of Hydrogen and Helium.
1170:Mirabel, I. F.; RodrĂguez, L. F. (1994-09-01).
811:Chen, Wen-Cong; Podsiadlowski, Philipp (2016).
339:. The compact, X-ray emitting, component is a
217:system where one of the components is either a
253:has revealed LMXBs in many distant galaxies.
1311:
673:"Mystery of Antimatter Source Solved – Maybe"
8:
1291:Ultraluminous X-ray Pulsar (ULXP) Catalogue
1286:Astronomy Cast episode 135: X-ray Astronomy
1003:The Astrophysical Journal Supplement Series
710:Introduction to Cataclysmic Variables (CVs)
469:regions. Microquasars are sometimes called
279:, but can sometimes be seen in the form of
152:
136:Accreting millisecond X-ray pulsars (AMXPs)
1318:
1304:
1296:
791:"Millisecond Pulsar Catalog - Black Sidus"
335:, or in some cases, a red supergiant or a
113:
89:
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957:
920:
883:
846:
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572:
558:
556:
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29:
550:
429:Artist's impression of the microquasar
60:), to the other component, called the
34:Artist's impression of an X-ray Binary
1172:"A superluminal source in the Galaxy"
1112:
1110:
1048:
1046:
1044:
724:"Accreting Millisecond X-ray Pulsars"
513:Centrifugal mechanism of acceleration
355:as it falls onto the compact object.
7:
1792:
133:or Super soft sources (SSXs), (SSXB)
147:Ultracompact X-ray binaries (UCXBs)
25:
503:, detected up to the High Energy
331:: usually an O or B star, a blue
88:escape per second from a typical
72:. The infalling matter releases
1791:
1782:
1781:
1533:Tolman–Oppenheimer–Volkoff limit
491:Noteworthy microquasars include
191:
171:Supergiant Fast X-ray Transients
142:Intermediate-mass X-ray binaries
1716:Fermi Gamma-ray Space Telescope
909:37th COSPAR Scientific Assembly
301:intermediate-mass X-ray binary
295:Intermediate-mass X-ray binary
74:gravitational potential energy
1:
1742:X-ray pulsar-based navigation
1721:Compton Gamma Ray Observatory
565:Compact Stellar X-ray Sources
413:binary if uninterrupted by a
403:red giant with a neutron core
53:(usually a relatively common
591:10.1017/CBO9780511536281.017
1711:Rossi X-ray Timing Explorer
1554:Gamma-ray burst progenitors
848:10.3847/0004-637X/830/2/131
754:10.1007/978-3-662-62110-3_4
1854:
1833:Astronomical X-ray sources
1767:Most massive neutron stars
1508:Quasi-periodic oscillation
1026:10.3847/0067-0049/222/2/15
976:10.1051/0004-6361:20077303
946:Astronomy and Astrophysics
1777:
1726:Chandra X-ray Observatory
1119:The Astrophysical Journal
1055:The Astrophysical Journal
817:The Astrophysical Journal
477:, often showing apparent
367:(not to be confused with
251:Chandra X-ray Observatory
165:Supergiant X-ray binaries
1493:Neutron-star oscillation
1382:Rotating radio transient
471:radio-jet X-ray binaries
289:thermonuclear explosions
153:High-mass X-ray binaries
131:Super soft X-ray sources
126:Symbiotic X-ray binaries
968:2007A&A...469..807L
872:The X-Ray Universe 2005
237:), or an evolved star (
114:Low-mass X-ray binaries
1747:Tempo software program
1284:Audio Cain/Gay (2009)
434:
317:high-mass X-ray binary
311:High-mass X-ray binary
233:, a degenerate dwarf (
105:
35:
1828:Semidetached binaries
1762:List of neutron stars
1757:The Magnificent Seven
428:
207:low-mass X-ray binary
201:Low-mass X-ray binary
120:Soft X-ray transients
103:
90:low-mass X-ray binary
45:that are luminous in
33:
27:Class of binary stars
18:Low-mass X-ray binary
1662:Thorne–Żytkow object
675:by John Borland 2008
347:. A fraction of the
64:, which is either a
1613:Neutron star merger
1473:Chandrasekhar limit
1440:Hulse–Taylor pulsar
1367:Soft gamma repeater
1280:2008AIPC.1010..252N
1248:2008AIPC.1010..252N
1188:1994Natur.371...46M
1141:2002ApJ...565.1107P
1077:2000ApJ...530L..93T
931:2008cosp...37.2892S
894:2006ESASP.604..165N
839:2016ApJ...830..131C
746:2021ASSL..461..143P
644:10.1038/nature06490
636:2008Natur.451..159W
583:2006csxs.book..623T
479:superluminal motion
104:Microquasar SS-433.
1657:Pulsar wind nebula
1635:Stellar black hole
509:Fermi acceleration
453:which is either a
435:
266:apparent magnitude
106:
36:
1805:
1804:
1586:Supernova remnant
1376:Ultra-long period
1273:10.1063/1.2945052
1256:10.1063/1.2945052
763:978-3-662-62110-3
600:978-0-521-82659-4
486:relativistic jets
475:relativistic jets
247:globular clusters
159:Be/X-ray binaries
16:(Redirected from
1845:
1795:
1794:
1785:
1784:
1559:Asteroseismology
1461:Fast radio burst
1320:
1313:
1306:
1297:
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1241:
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1196:10.1038/371046a0
1167:
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1132:astro-ph/0107261
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1068:astro-ph/0001013
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885:astro-ph/0511088
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686:"A game-changer"
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630:(7175): 159–62.
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574:astro-ph/0303456
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84:An estimated 10
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1468:Bondi accretion
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1372:Anomalous X-ray
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1182:(6492): 46–48.
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337:Wolf–Rayet star
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41:are a class of
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1222:External links
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1085:10.1086/312496
1061:(2): L93–L96.
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451:compact object
449:surrounding a
447:accretion disk
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384:X-ray bursters
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285:X-ray bursters
277:X-ray bursters
270:accretion disk
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1640:Related links
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985:
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937:
932:
928:
923:
918:
914:
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895:
891:
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878:(2006): 165.
877:
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849:
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840:
836:
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826:
822:
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769:
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751:
747:
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729:
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718:
715:
712:, NASA, 2006.
711:
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399:
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389:
388:X-ray pulsars
385:
381:
380:X-ray pulsars
376:
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342:
338:
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282:
281:X-ray pulsars
278:
273:
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267:
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252:
248:
244:
240:
236:
232:
231:main sequence
228:
224:
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190:
188:
187:X-ray pulsars
185:
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63:
59:
56:
55:main sequence
52:
48:
44:
40:
32:
19:
1823:Binary stars
1564:Compact star
1538:Urca process
1528:Timing noise
1513:Relativistic
1408:X-ray binary
1407:
1403:X-ray pulsar
1327:Neutron star
1229:
1179:
1175:
1165:
1122:
1118:
1058:
1054:
1006:
1002:
992:
949:
945:
939:
912:
908:
902:
875:
871:
865:
820:
816:
806:
795:. Retrieved
793:. 2013-09-30
785:
775:, retrieved
727:
717:
705:
693:. Retrieved
689:
680:
668:
627:
623:
617:
564:
530:LS I +61 303
497:GRS 1915+105
490:
483:
470:
463:solar masses
459:neutron star
438:
436:
411:neutron star
407:neutron star
405:or a single
400:
392:stellar wind
377:
357:
349:stellar wind
341:neutron star
320:
316:
314:
304:
300:
298:
274:
255:
223:neutron star
210:
206:
204:
192:Microquasars
107:
83:
66:neutron star
61:
50:
43:binary stars
38:
37:
1623:White dwarf
1608:Microquasar
1574:Exotic star
1503:Pulsar kick
1425:Millisecond
1341:Radio-quiet
1125:(2): 1107.
690:www.eso.org
525:4U 0614+091
439:microquasar
421:Microquasar
325:binary star
235:white dwarf
215:binary star
1812:Categories
1752:Astropulse
1667:QCD matter
1647:Radio star
1618:Quark-nova
1569:Quark star
1518:Rp-process
1449:Properties
1016:1512.00778
952:(2): 807.
830:1608.02088
823:(2): 131.
797:2022-06-16
777:2022-06-16
546:References
505:gamma rays
501:Cygnus X-1
455:black hole
396:Roche lobe
373:4U 1700-37
361:Cygnus X-1
345:black hole
333:supergiant
227:Roche lobe
219:black hole
70:black hole
1702:Satellite
1676:Discovery
1598:Hypernova
1581:Supernova
1523:Starquake
1239:0801.3863
1204:0028-0836
1035:118833989
1009:(2): 15.
959:0707.0544
922:0809.3157
857:118475703
772:118471125
737:1206.2727
415:supernova
258:radiation
243:Milky Way
239:red giant
86:positrons
1787:Category
1603:Kilonova
1430:Be/X-ray
1362:Magnetar
1264:18941968
1157:16381236
1101:17772120
1093:10655173
984:14673570
915:: 2892.
652:18185581
609:18856214
519:See also
386:. These
382:and not
365:Vela X-1
161:(BeXRBs)
155:(HMXBs)
144:(IMXBs)
116:(LMXBs)
62:accretor
1797:Commons
1547:Related
1498:Optical
1456:Blitzar
1435:Spin-up
1276:Bibcode
1244:Bibcode
1212:4347263
1184:Bibcode
1137:Bibcode
1073:Bibcode
964:Bibcode
927:Bibcode
890:Bibcode
835:Bibcode
742:Bibcode
695:15 July
660:4333175
632:Bibcode
579:Bibcode
371:), and
323:) is a
249:. The
213:) is a
178:Others
173:(SFXTs)
167:(SGXBs)
1483:Glitch
1398:Binary
1346:Pulsar
1262:
1210:
1202:
1176:Nature
1155:
1099:
1091:
1033:
982:
855:
770:
760:
658:
650:
624:Nature
607:
597:
540:Quasar
535:SS 433
493:SS 433
443:quasar
431:SS 433
369:Vela X
353:X-rays
283:. The
262:X-rays
122:(SXTs)
78:fusion
47:X-rays
1735:Other
1683:LGM-1
1334:Types
1260:S2CID
1234:arXiv
1208:S2CID
1153:S2CID
1127:arXiv
1097:S2CID
1063:arXiv
1031:S2CID
1011:arXiv
980:S2CID
954:arXiv
917:arXiv
880:arXiv
853:S2CID
825:arXiv
768:S2CID
732:arXiv
656:S2CID
605:S2CID
569:arXiv
467:X-ray
457:or a
51:donor
1418:List
1200:ISSN
1089:PMID
758:ISBN
697:2019
648:PMID
595:ISBN
511:and
394:and
329:star
321:HMXB
305:IMXB
211:LMXB
58:star
1269:doi
1252:doi
1192:doi
1180:371
1145:doi
1123:565
1081:doi
1059:530
1021:doi
1007:222
972:doi
950:469
876:604
843:doi
821:830
750:doi
640:doi
628:451
587:doi
515:).
343:or
299:An
260:in
221:or
68:or
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1250:.
1242:.
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1174:.
1151:.
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1109:^
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1043:^
1029:.
1019:.
1005:.
1001:.
978:.
970:.
962:.
948:.
925:.
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911:.
888:.
874:.
851:.
841:.
833:.
819:.
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577:.
553:^
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437:A
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315:A
205:A
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892::
882::
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845::
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800:.
752::
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699:.
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642::
634::
611:.
589::
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319:(
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209:(
20:)
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