186:
field plays a fundamental role in their formation. Absorption features may then provide a powerful diagnostics for the strength of the surface field. At present, two main explanations for their origin have been suggested: either proton cyclotron resonances or atomic transitions in light elements. For the two sources in which a spin-down measure is available, the values of B obtained from spin-down assuming magnetodipolar braking are in reasonable agreement with those inferred from the line energy. Once the nature of the lines has been settled and if an independent measurement of the magnetic field is available (e.g. through spin-down), a measure of the gravitational redshift will be possible, paving the way to the simultaneous determination of both the star mass and radius.
128:. The continuous monitoring revealed however that the source underwent conspicuous changes in the period 2001–2003. In particular, while the total flux stayed more or less constant, the blackbody temperature steadily increased, going from about 86 to over 90 eV. This was accompanied by a change of the pulse profile, with an increase of the pulsed fraction. More recently this trend seems to have reversed. Starting from 2004, the temperature decreased, and there are hints that the overall evolution may be cyclic, with a period of about 10 years.
2005:
2065:
2089:
2015:
2041:
2077:
2053:
174:, a local group of stars with an age of about 30–50 million years formed by massive stars. Reconstruction of trajectories of neutron stars confirmed this conclusion. In the solar vicinity, these neutron stars outnumber radio pulsars of the same age. This means that the Magnificent Seven-like objects may be one of the most typical young
626:
Despite many attempts, no radio emission has been detected from these sources. The preliminary results from latest deep search with the GBT telescope are presented by
Kondratiev et al. There are claims that some signal was detected at very low frequencies, but these results are not very certain and
111:
shapes are quasisinusoidal and single-peaked. However, RX J1308.6+2127 displays a double-peaked light curve, and in RX J0420.0-5022 there is some evidence for a skewness in the pulse profile, with a slower rise and faster decline. Rather counter-intuitively, the spectrum of both RX J0720.4-3125 and
185:
XMM-Newton's observations made it possible to detect wide absorption features in spectra of several of the
Magnificent Seven. Although their origin is not clear yet (see Haberl (2006) for references and more detailed description of the results), it is almost certain that the stars' strong magnetic
166:
are known. The distance to the sources is about 161 parsecs. Similar data is obtained for the second brightest object RX J0720.4-3125. The distance is about 330 parsecs. Projected velocities are approximately 280 kilometers per second (km/s) and 115 km/s, respectively. These data allow
610:
can be determined by spectral analysis, the previous relation immediately yields the star radius. Reality is somewhat more complicated, but this oversimplified analysis captures the essence of what is needed in order to measure the neutron star radius: distance, flux and surface temperature.
428:
Data for the table were partly taken from Kaplan (2008), partly from a review by R. Turolla (2009), and partly from other sources. Temperature estimates vary slightly in different publications. The source RX J0720.4-3125 is variable in temperature and pulsed fraction.
611:
Observing the star thermal emission is therefore crucial. Among all thermally emitting neutrons stars the
Magnificent Seven are the only ones with a purely blackbody spectrum. Their clean thermal emission, unmarred by contamination from
115:
A coherent timing solution has been recently obtained for RX J0720.4-3125 and RX J1308.6+2127. The periods are changing by 7 × 10 seconds per second and 10 s/s, respectively. The derived dipolar field is 2–3 × 10
441:(EOS) of matter at supra-nuclear densities. The most direct way of constraining the EOS is to measure simultaneously the neutron star mass and radius. If a neutron star emits blackbody radiation from its surface of radius
91:
All seven are recognized to be relatively close by (less than a few hundred parsecs), middle-age (several hundred thousand years) isolated neutron stars emitting soft X-rays due to cooling. The cooling is confirmed by the
123:
For a long time the Seven were considered to be steady sources, to the point that RX J0720.4-3125 was included among the calibration sources for the EPIC and RGS instruments on board the orbital X-ray telescope
565:
437:
The seven objects seem to be the best laboratory to study neutron star atmospheres and, probably, internal structure. The holy grail of neutron star astrophysics is the determination of the
1926:
104:); for comparison, the Sun's corona has a temperature of about 5 megakelvins). At least six out of the seven show spin periods in the range of approximately 3 to 12 seconds.
1511:
167:
astronomers to reconstruct the stars' trajectory and so identify the site of their birth. Distance estimates to other sources can be found in
Posselt et al. (2007)
608:
588:
499:
479:
459:
75:. However, it was soon shown that MS 0317.7-6647 is, in fact, not a neutron star. Then in 2001 a new object fitting this classification was discovered:
1766:
890:
Hohle, M. M.; et al. (2009). "Spectral and temporal variations of the isolated neutron star RX J0720.4-3125: New XMM-Newton observations".
1551:
1409:
1031:
Kaplan, D. L.; van
Kerkwijk, M. H. (2005b). "A Coherent Timing Solution for the Nearby Isolated Neutron Star RX J1308.6+2127/RBS 1223".
2114:
507:
1949:
984:
Kaplan, D. L.; van
Kerkwijk, M. H. (2005a). "A Coherent Timing Solution for the Nearby Isolated Neutron Star RX J0720.4-3125".
1117:
Kondratiev, V. I.; et al. (2008). "A Search for Pulsed and Bursty Radio
Emission from X-ray Dim Isolated Neutron Stars".
1975:
1954:
2031:
937:
Kaplan, D. L.; van
Kerkwijk, M. H.; Anderson, J. (2002). "The Parallax and Proper Motion of RX J1856.5-3754 Revisited".
1895:
1944:
1787:
76:
1741:
1544:
1959:
135:. There are other types of young isolated neutron stars which are different from standard radio pulsars, such as
131:
The
Magnificent Seven represent a large class of young neutron stars with many properties different from normal
2018:
1756:
1726:
1615:
1574:
1512:"Physicists May Have Found Dark Matter: X-rays Surrounding "Magnificent 7" May Be Traces of Theorized Particle"
144:
1673:
1419:
Walter, Frederick M.; Wolk, Scott J.; Neuhäuser, Ralph (1996). "Discovery of a nearby isolated neutron star".
1456:
Zampieri, L.; et al. (2001). "1RXS J214303.7+065419/RBS 1774: A new
Isolated Neutron Star candidate".
2109:
2008:
1605:
636:
159:
140:
1651:
1537:
843:
Haberl, Frank (2007). "The magnificent seven: Magnetic fields and surface temperature distributions".
1873:
1861:
1668:
1475:
1428:
1389:
1372:
1325:
1278:
1216:
1169:
1132:
1097:
1050:
1003:
956:
909:
862:
101:
68:
60:
72:
47:, which was discovered by Walter et al. in 1992, and confirmed as a neutron star in 1996. The term
2093:
1846:
1824:
1706:
1600:
136:
158:
Some of the seven have very weak optical counterparts. For the brightest one (RX J1856-3754), the
2081:
2069:
1890:
1868:
1716:
1658:
1491:
1465:
1444:
1362:
1341:
1315:
1294:
1268:
1245:
1232:
1206:
1185:
1148:
1122:
1087:
1066:
1040:
1019:
993:
972:
946:
925:
899:
878:
852:
152:
1980:
1819:
1746:
1405:
1306:
Potekhin, Alexander Y.; De Luca, Andrea; Pons, José (2015). "Neutron Stars—Thermal Emitters".
620:
438:
79:. Since 2001, no new good candidates have appeared. All seven sources were discovered by the
56:
52:
2045:
1792:
1694:
1483:
1479:
1436:
1397:
1333:
1286:
1282:
1224:
1220:
1177:
1173:
1140:
1105:
1058:
1011:
964:
917:
913:
870:
866:
1160:
Malofeev, V. M.; Malov, O. I.; Teplykh, D. A. (2007). "Radio emission from AXP and XDINS".
1711:
1701:
1663:
1353:
Treves, A.; et al. (2001). "The Magnificent Seven: Close-by Cooling Neutron Stars?".
64:
44:
1432:
1393:
1376:
1329:
1136:
1101:
1054:
1007:
960:
1731:
1721:
593:
573:
484:
464:
444:
148:
1197:
Popov, S. B.; et al. (2003). "Young isolated neutron stars from the Gould Belt".
2103:
1921:
1916:
1885:
1646:
1631:
1189:
612:
179:
175:
163:
132:
97:
1495:
1345:
1298:
1236:
1152:
1070:
1023:
976:
882:
2057:
1797:
1771:
1641:
1636:
1560:
1448:
929:
117:
20:
1078:
Kaplan, David L.; et al. (2008). "Nearby, Thermally Emitting Neutron Stars".
921:
1487:
1228:
1856:
1841:
1807:
1736:
1401:
1384:
Turolla, Roberto (2009). "Isolated Neutron Stars: The Challenge of Simplicity".
170:
Population synthesis studies show that the Magnificent Seven are related to the
108:
1259:
Posselt, B.; et al. (2007). "The Magnificent Seven in the dusty prairie".
1985:
1900:
1880:
1851:
1802:
1751:
1337:
1290:
1181:
874:
171:
125:
93:
1831:
1814:
1388:. Astrophysics and Space Science Library. Vol. 357. pp. 141–163.
1836:
1595:
1470:
1367:
1273:
1250:
1211:
1045:
998:
951:
857:
1689:
1144:
1109:
1761:
1579:
1440:
616:
24:
2052:
1062:
1015:
968:
1320:
1127:
1092:
904:
816:
80:
703:
1533:
1529:
96:
shapes of their spectra. Typical temperatures are about 50–100
560:{\displaystyle F=\sigma T^{4}\left({\tfrac {R}{D}}\right)^{2}}
1121:. AIP Conference Series. Vol. 983. pp. 348–350.
761:
19:
is the informal name of a group of isolated young cooling
783:
772:
692:
27:
from Earth. These objects are also known under the names
155:. Some of them can be related to the Magnificent Seven.
1927:
Timeline of white dwarfs, neutron stars, and supernovae
739:
623:, makes these sources ideal targets for such a study.
536:
178:
with a galactic birth rate larger than that of normal
51:
was initially applied to the sources RX J1856.5-3754,
2029:
596:
576:
510:
487:
467:
447:
827:
120:
and the spin-down ages are 2 and 1.5 million years.
1968:
1935:
1909:
1780:
1682:
1624:
1588:
1567:
725:
714:
681:
670:
602:
582:
559:
493:
473:
453:
1244:Popov, S. B. (2006). "The Zoo of Neutron Stars".
112:RX J1308.6+2127 becomes harder at pulse minimum.
655:
653:
651:
735:
733:
659:
1545:
31:(X-ray Dim Isolated Neutron Stars) or simply
8:
1552:
1538:
1530:
193:
1469:
1366:
1319:
1272:
1249:
1210:
1126:
1091:
1044:
997:
950:
903:
856:
595:
575:
551:
535:
524:
509:
486:
466:
446:
407:−50° 22′ 48.1″
379:−41° 22′ 30.9″
351:+06° 54′ 17.0″
321:+21° 27′ 06.8″
291:+32° 49′ 18.1″
261:−31° 25′ 50.2″
233:−37° 54′ 30.5″
43:The first to fit this classification was
1119:40 Years of Pulsars: Millisecond Pulsars
762:Kaplan, van Kerkwijk & Anderson 2002
2036:
805:
647:
794:
750:
7:
2014:
828:Malofeev, Malov & Teplykh 2007
14:
682:Walter, Wolk & Neuhäuser 1996
671:Potekhin, De Luca & Pons 2015
2087:
2075:
2063:
2051:
2039:
2013:
2004:
2003:
1767:Tolman–Oppenheimer–Volkoff limit
481:, the received flux at distance
1950:Fermi Gamma-ray Space Telescope
1080:Astrophysics of Compact Objects
726:Kaplan & van Kerkwijk 2005b
715:Kaplan & van Kerkwijk 2005a
1261:Astrophysics and Space Science
1162:Astrophysics and Space Science
845:Astrophysics and Space Science
77:1RXS J214303.7+065419/RBS 1774
1:
1976:X-ray pulsar-based navigation
1955:Compton Gamma Ray Observatory
23:at a distance of 120 to 500
1945:Rossi X-ray Timing Explorer
1788:Gamma-ray burst progenitors
1402:10.1007/978-3-540-76965-1_7
922:10.1051/0004-6361/200810812
461:at homogeneous temperature
100:(57.5–115 kilokelvins (see
2131:
1742:Quasi-periodic oscillation
1488:10.1051/0004-6361:20011151
1458:Astronomy and Astrophysics
1229:10.1051/0004-6361:20030680
1199:Astronomy and Astrophysics
892:Astronomy and Astrophysics
2115:Radio-quiet neutron stars
1999:
1960:Chandra X-ray Observatory
1386:Neutron Stars and Pulsars
1338:10.1007/s11214-014-0102-2
1291:10.1007/s10509-007-9344-8
1182:10.1007/s10509-007-9341-y
1033:The Astrophysical Journal
986:The Astrophysical Journal
939:The Astrophysical Journal
875:10.1007/s10509-007-9342-x
145:rotating radio transients
1727:Neutron-star oscillation
1616:Rotating radio transient
615:activity, a surrounding
190:Physical characteristics
1480:2001A&A...378L...5Z
1283:2007Ap&SS.308..171P
1221:2003A&A...406..111P
1174:2007Ap&SS.308..211M
914:2009A&A...498..811H
867:2007Ap&SS.308..181H
141:anomalous X-ray pulsars
1981:Tempo software program
817:Kondratiev et al. 2008
637:Calvera (X-ray source)
627:require confirmation.
604:
584:
561:
495:
475:
455:
160:trigonometric parallax
1991:The Magnificent Seven
1308:Space Science Reviews
605:
585:
562:
496:
476:
456:
17:The Magnificent Seven
1896:Thorne–Żytkow object
1355:X-Ray Astronomy 2000
704:Zampieri et al. 2001
594:
574:
508:
485:
465:
445:
220:Age (million years)
137:soft gamma repeaters
102:Electron temperature
1847:Neutron star merger
1707:Chandrasekhar limit
1674:Hulse–Taylor pulsar
1601:Soft gamma repeater
1433:1996Natur.379..233W
1394:2009ASSL..357..141T
1377:2001ASPC..234..225T
1330:2015SSRv..191..171P
1137:2008AIPC..983..348K
1102:2008AIPC..968..129K
1055:2005ApJ...635L..65K
1008:2005ApJ...628L..45K
961:2002ApJ...571..447K
773:Posselt et al. 2007
1891:Pulsar wind nebula
1869:Stellar black hole
693:Treves et al. 2001
660:Kaplan et al. 2008
600:
580:
557:
545:
491:
471:
451:
153:supernova remnants
2027:
2026:
1820:Supernova remnant
1610:Ultra-long period
1518:. 15 January 2021
1427:(6562): 233–235.
1411:978-3-540-76964-4
1145:10.1063/1.2900180
1110:10.1063/1.2840384
784:Popov et al. 2003
740:Hohle et al. 2009
621:supernova remnant
603:{\displaystyle T}
583:{\displaystyle D}
544:
494:{\displaystyle D}
474:{\displaystyle T}
454:{\displaystyle R}
439:equation of state
426:
425:
49:Magnificent Seven
2122:
2092:
2091:
2090:
2080:
2079:
2078:
2068:
2067:
2066:
2056:
2055:
2044:
2043:
2042:
2035:
2017:
2016:
2007:
2006:
1793:Asteroseismology
1695:Fast radio burst
1554:
1547:
1540:
1531:
1526:
1524:
1523:
1499:
1473:
1471:astro-ph/0108456
1452:
1441:10.1038/379233a0
1415:
1380:
1370:
1368:astro-ph/0011564
1349:
1323:
1314:(1–4): 171–206.
1302:
1276:
1274:astro-ph/0609275
1267:(1–4): 171–179.
1255:
1253:
1251:astro-ph/0610593
1240:
1214:
1212:astro-ph/0304141
1193:
1168:(1–4): 211–216.
1156:
1130:
1113:
1095:
1074:
1048:
1046:astro-ph/0511084
1027:
1001:
999:astro-ph/0506419
980:
954:
952:astro-ph/0111174
933:
907:
886:
860:
858:astro-ph/0609066
851:(1–4): 181–190.
830:
825:
819:
814:
808:
803:
797:
792:
786:
781:
775:
770:
764:
759:
753:
748:
742:
737:
728:
723:
717:
712:
706:
701:
695:
690:
684:
679:
673:
668:
662:
657:
609:
607:
606:
601:
589:
587:
586:
581:
570:So, if distance
566:
564:
563:
558:
556:
555:
550:
546:
537:
529:
528:
500:
498:
497:
492:
480:
478:
477:
472:
460:
458:
457:
452:
404:
376:
348:
318:
288:
258:
230:
194:
2130:
2129:
2125:
2124:
2123:
2121:
2120:
2119:
2100:
2099:
2098:
2088:
2086:
2076:
2074:
2064:
2062:
2050:
2040:
2038:
2030:
2028:
2023:
1995:
1964:
1937:
1931:
1905:
1776:
1712:Gamma-ray burst
1702:Bondi accretion
1678:
1620:
1606:Anomalous X-ray
1584:
1563:
1558:
1521:
1519:
1510:
1507:
1505:Further reading
1502:
1455:
1418:
1412:
1383:
1352:
1305:
1258:
1243:
1196:
1159:
1116:
1077:
1030:
983:
936:
889:
842:
838:
833:
826:
822:
815:
811:
804:
800:
793:
789:
782:
778:
771:
767:
760:
756:
749:
745:
738:
731:
724:
720:
713:
709:
702:
698:
691:
687:
680:
676:
669:
665:
658:
649:
645:
633:
592:
591:
572:
571:
531:
530:
520:
506:
505:
483:
482:
463:
462:
443:
442:
435:
402:
374:
346:
342:
316:
312:
286:
282:
256:
228:
217:line energy, eV
216:
212:Temperature, eV
206:Spin Periods, s
200:Right Ascension
192:
149:compact objects
89:
87:Characteristics
69:RX J0420.0-5022
65:RX J0720.4-3125
61:RX J0806.4-4132
45:RX J1856.5-3754
41:
12:
11:
5:
2128:
2126:
2118:
2117:
2112:
2102:
2101:
2097:
2096:
2084:
2072:
2060:
2048:
2025:
2024:
2022:
2021:
2011:
2000:
1997:
1996:
1994:
1993:
1988:
1983:
1978:
1972:
1970:
1966:
1965:
1963:
1962:
1957:
1952:
1947:
1941:
1939:
1933:
1932:
1930:
1929:
1924:
1919:
1913:
1911:
1907:
1906:
1904:
1903:
1898:
1893:
1888:
1883:
1878:
1877:
1876:
1866:
1865:
1864:
1854:
1849:
1844:
1839:
1834:
1829:
1828:
1827:
1822:
1812:
1811:
1810:
1805:
1795:
1790:
1784:
1782:
1778:
1777:
1775:
1774:
1769:
1764:
1759:
1754:
1749:
1744:
1739:
1734:
1729:
1724:
1722:Neutron matter
1719:
1714:
1709:
1704:
1699:
1698:
1697:
1686:
1684:
1680:
1679:
1677:
1676:
1671:
1666:
1661:
1656:
1655:
1654:
1649:
1644:
1634:
1628:
1626:
1625:Binary pulsars
1622:
1621:
1619:
1618:
1613:
1612:
1611:
1608:
1603:
1592:
1590:
1589:Single pulsars
1586:
1585:
1583:
1582:
1577:
1571:
1569:
1565:
1564:
1559:
1557:
1556:
1549:
1542:
1534:
1528:
1527:
1506:
1503:
1501:
1500:
1453:
1416:
1410:
1381:
1350:
1303:
1256:
1241:
1194:
1157:
1114:
1075:
1063:10.1086/499241
1028:
1016:10.1086/432536
981:
969:10.1086/339879
934:
887:
839:
837:
834:
832:
831:
820:
809:
798:
787:
776:
765:
754:
743:
729:
718:
707:
696:
685:
674:
663:
646:
644:
641:
640:
639:
632:
629:
613:magnetospheric
599:
579:
568:
567:
554:
549:
543:
540:
534:
527:
523:
519:
516:
513:
490:
470:
450:
434:
431:
424:
423:
420:
417:
414:
411:
408:
405:
400:
396:
395:
392:
389:
386:
383:
380:
377:
372:
368:
367:
364:
361:
358:
355:
352:
349:
344:
338:
337:
334:
331:
328:
325:
322:
319:
314:
308:
307:
304:
301:
298:
295:
292:
289:
284:
278:
277:
274:
271:
268:
265:
262:
259:
254:
250:
249:
246:
243:
240:
237:
234:
231:
226:
222:
221:
218:
213:
210:
207:
204:
201:
198:
191:
188:
147:, and central
88:
85:
73:MS 0317.7-6647
40:
37:
13:
10:
9:
6:
4:
3:
2:
2127:
2116:
2113:
2111:
2110:Neutron stars
2108:
2107:
2105:
2095:
2085:
2083:
2073:
2071:
2061:
2059:
2054:
2049:
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1938:investigation
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1886:Pulsar planet
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1874:Related links
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1862:Related links
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590:is known and
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552:
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541:
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180:radio pulsars
177:
176:neutron stars
173:
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164:proper motion
161:
156:
154:
150:
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142:
138:
134:
133:radio pulsars
129:
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110:
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98:electronvolts
95:
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84:
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78:
74:
70:
66:
62:
58:
54:
50:
46:
38:
36:
34:
30:
26:
22:
21:neutron stars
18:
2094:Solar System
1990:
1798:Compact star
1772:Urca process
1762:Timing noise
1747:Relativistic
1642:X-ray binary
1637:X-ray pulsar
1561:Neutron star
1520:. Retrieved
1516:SciTechDaily
1515:
1461:
1457:
1424:
1420:
1385:
1358:
1354:
1311:
1307:
1264:
1260:
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1198:
1165:
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1036:
1032:
989:
985:
942:
938:
895:
891:
848:
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823:
812:
806:Turolla 2009
801:
790:
779:
768:
757:
746:
721:
710:
699:
688:
677:
666:
625:
569:
436:
427:
197:Source, RX J
184:
169:
157:
130:
122:
114:
106:
90:
48:
42:
32:
28:
16:
15:
2082:Outer space
2070:Spaceflight
1857:White dwarf
1842:Microquasar
1808:Exotic star
1737:Pulsar kick
1659:Millisecond
1575:Radio-quiet
1205:: 111–117.
1086:: 129–136.
795:Haberl 2007
403:04 20 01.95
399:0420.0–5022
375:08 06 23.40
371:0806.4−4123
347:21 43 03.30
341:2143.0+0654
317:13 08 48.27
311:1308.6+2127
287:16 05 18.52
281:1605.3+3249
257:07 20 24.96
253:0720.4−3125
229:18 56 35.11
225:1856.5−3754
209:Amplitude/2
203:Declination
109:light curve
83:satellite.
2104:Categories
1986:Astropulse
1901:QCD matter
1881:Radio star
1852:Quark-nova
1803:Quark star
1752:Rp-process
1683:Properties
1522:2021-01-27
1039:(1): L65.
992:(1): L45.
945:(1): 447.
898:(3): 811.
751:Popov 2006
643:References
343:(RBS 1774)
313:(RBS 1223)
283:(RBS 1556)
215:Absorption
172:Gould Belt
126:XMM-Newton
94:black body
2046:Astronomy
1936:Satellite
1910:Discovery
1832:Hypernova
1815:Supernova
1757:Starquake
1464:: L5–L9.
1321:1409.7666
1190:120490290
1128:0710.1648
1093:0801.1143
905:0810.5319
518:σ
2009:Category
1837:Kilonova
1664:Be/X-ray
1596:Magnetar
1496:16572677
1346:53365097
1299:16718273
1237:16094637
1153:15026449
1071:14439352
1024:16973889
977:10718657
883:15013359
631:See also
433:Research
2032:Portals
2019:Commons
1781:Related
1732:Optical
1690:Blitzar
1669:Spin-up
1476:Bibcode
1449:4313699
1429:Bibcode
1390:Bibcode
1373:Bibcode
1361:: 225.
1326:Bibcode
1279:Bibcode
1217:Bibcode
1170:Bibcode
1133:Bibcode
1098:Bibcode
1051:Bibcode
1004:Bibcode
957:Bibcode
930:1808233
910:Bibcode
863:Bibcode
836:Sources
360:102–104
57:RBS1223
53:RBS1556
39:History
25:parsecs
1717:Glitch
1632:Binary
1580:Pulsar
1494:
1447:
1421:Nature
1408:
1344:
1297:
1235:
1188:
1151:
1069:
1022:
975:
928:
881:
617:nebula
2058:Stars
1969:Other
1917:LGM-1
1568:Types
1492:S2CID
1466:arXiv
1445:S2CID
1363:arXiv
1342:S2CID
1316:arXiv
1295:S2CID
1269:arXiv
1246:arXiv
1233:S2CID
1207:arXiv
1186:S2CID
1149:S2CID
1123:arXiv
1088:arXiv
1067:S2CID
1041:arXiv
1020:S2CID
994:arXiv
973:S2CID
947:arXiv
926:S2CID
900:arXiv
879:S2CID
853:arXiv
422:1.98
394:3.24
382:11.37
366:3.65
336:1.46
324:10.31
300:93–96
276:1.90
270:85–87
248:3.76
242:60–62
118:Gauss
81:ROSAT
29:XDINS
1652:List
1406:ISBN
501:is:
410:3.45
354:9.44
264:8.39
239:1.5%
236:7.06
162:and
107:The
71:and
33:XINS
1484:doi
1462:378
1437:doi
1425:379
1398:doi
1359:234
1334:doi
1312:191
1287:doi
1265:308
1225:doi
1203:406
1178:doi
1166:308
1141:doi
1106:doi
1084:968
1059:doi
1037:635
1012:doi
990:628
965:doi
943:571
918:doi
896:498
871:doi
849:308
619:or
419:330
413:13%
391:460
363:700
333:300
330:102
327:18%
303:450
294:???
273:270
267:11%
151:in
2106::
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1002:.
988:.
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894:.
877:.
869:.
861:.
847:.
732:^
650:^
416:45
388:92
385:6%
357:4%
306:?
245:no
182:.
143:,
139:,
67:,
63:,
59:,
55:,
35:.
2034::
1553:e
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1112:.
1108::
1100::
1090::
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1061::
1053::
1043::
1026:.
1014::
1006::
996::
979:.
967::
959::
949::
932:.
920::
912::
902::
885:.
873::
865::
855::
598:T
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553:2
548:)
542:D
539:R
533:(
526:4
522:T
515:=
512:F
489:D
469:T
449:R
297:–
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