455:. An object that overflows its Roche lobe will lose mass to its more massive companion. Such a scenario is used to explain how the companion in this system, once likely a star, lost so much mass to become a planet massed object. The accretion of this material also explains the "spin-up" of the millisecond pulsar, so that it can have such a short rotational period. It is possible that PSR J1311–3430 will eventually completely vaporize its companion, and become a solitary millisecond pulsar.
2253:
463:
The identification of a millisecond pulsar via a blind search of gamma-ray data alone provides hope that other gamma-ray sources with unknown origin can be identified as millisecond pulsars, especially given that radio pulses from PSR J1311–3430 were detected less than 10% of the time observed. Among
402:
The detection and timing of the gamma ray pulsations was used to determine the spin period of the pulsar to be 2.5 milliseconds. The presence of the companion to the pulsar causes very slight variations in the time at which these pulses appear to be emitted, meaning precise timing allows the minimum
381:
data, led by Holger
Pletsch, revealed that 2FGL J1317.7–3429 was a millisecond pulsar with a 2.5 millisecond period, the first example of a millisecond pulsar detected via gamma-ray pulsations. With the discovery of the pulsations, it was named PSR J1311–3430, with "PSR" denoting pulsar. Follow-up
28:
34:
33:
30:
29:
35:
32:
450:
detected. Variations in the optical brightness reveal large temperature variations in the companion. Modeling of the variations indicate strong heating of the companion by the pulsar, and that the companion nearly fills its
220:
of 93.8 minutes. The system is explained by a model where mass from the low mass companion was transferred on to the pulsar, increasing the mass of the pulsar and decreasing its period. These systems are known as
343:. Other point sources, however, remained a mystery, as they had no known counterpart at other wavelengths. One such unidentified source was 2FGL J1317.7–3429 (so named because it was in a catalog of
795:
Romani; Filippenko; Silverman; Bradley Cenko; Jochen
Greiner; Arne Rau; Jonathan Elliott; Pletsch (2012). "PSR J1311-3430: A Heavyweight Neutron Star with a Flyweight Helium Companion".
358:
In an effort to detect a new origin of gamma-ray emission, Roger Romani performed a deep search for counterparts of the brightest unidentified gamma-ray sources. His search uncovered
489:
432:
289:
258:
31:
491:. This mass determination for the pulsar supports the existing notion that these systems are hosts to pulsars with large masses, and also provides constraints on the
697:
Ray; Ransom; Cheung; Giroletti; Cognard; Camilo; Bhattacharyya; Roy; Romani (2012). "Radio
Detection of the Fermi LAT Blind Search Millisecond Pulsar J1311-3430".
229:, and may eventually lead to the companion being completely vaporized. Among systems like these, the orbital period of PSR J1311–3430 is the shortest ever found.
366:
emission at the same location as 2FGL J1317.7–3429 that changed amplitude with a period of roughly 1.5 hours, and suggested that the origin could be a
264:). Though there is considerable uncertainty in this estimate, the minimum mass for the pulsar that the authors find adequately fits the data is 2.15
304:
216:
discovered pulsed gamma ray emission. The pulsar has a helium-dominated companion much less massive than itself, and the two are in an orbit with a
205:
370:
in a black-widow-type system, but also noted that this would need to be confirmed by the discovery of pulsations in the gamma-ray data or at
464:
known black-widow-type binary pulsar systems, PSR J1311–3430 has the shortest orbital period, and a mass constrained to be larger than 2.1
867:
1871:
615:
308:
213:
52:
892:
2275:
2218:
1629:
386:
that were only visible for <10% of the time the source was observed. The authors suggested that the pulses could be
887:
1104:
876:
1654:
860:
1490:
340:
101:
2078:
2073:
1973:
1262:
1071:
512:
404:
2200:
1937:
1207:
814:
765:
716:
659:
383:
640:
Pletsch, H. J.; et al. (2012). "Binary
Millisecond Pulsar Discovery via Gamma-Ray Pulsations".
320:
185:
292:
2280:
2256:
1790:
1785:
1780:
853:
830:
804:
781:
755:
732:
706:
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649:
367:
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226:
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201:
467:
410:
267:
236:
1046:
1041:
1016:
1011:
911:
675:
492:
377:
Within a few months, this conjecture was confirmed. A blind search of more than four years of
48:
2169:
1902:
956:
934:
929:
924:
822:
773:
724:
667:
359:
141:
2159:
986:
348:
73:
1679:
818:
769:
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663:
2187:
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1252:
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1031:
981:
971:
951:
946:
919:
217:
159:
826:
777:
728:
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1217:
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976:
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230:
60:
834:
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2144:
1912:
1813:
1710:
1061:
1056:
1051:
1036:
1026:
1006:
1001:
966:
439:
382:
radio observations were able to also detect intermittent radio pulsations with the
121:
335:
were at the same locations as previously known objects from observations at other
2093:
1775:
1770:
1765:
1760:
1755:
1750:
1745:
1740:
1735:
1730:
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1335:
1325:
1280:
1157:
1152:
1147:
1142:
1137:
1021:
996:
991:
371:
352:
323:
observed emission on large scales in the sky, associated with emission from the
148:
86:
2195:
2154:
2149:
2139:
1435:
1425:
1420:
1410:
1400:
1340:
1320:
1315:
1310:
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1132:
1127:
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1117:
1112:
1094:
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452:
391:
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261:
128:
845:
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2001:
1907:
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1603:
1598:
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1578:
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1568:
1563:
1558:
1553:
1548:
1543:
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1533:
1528:
1523:
1518:
1513:
1508:
1480:
1475:
1470:
1465:
1460:
1455:
1450:
1445:
1440:
1430:
1415:
1405:
1395:
1390:
1385:
1380:
1375:
1370:
1365:
1360:
1355:
1345:
1330:
1305:
1300:
1295:
1290:
1285:
1275:
1270:
1232:
1227:
1222:
1177:
671:
324:
316:
209:
204:
found via gamma-ray pulsations. The source was originally identified by the
65:
679:
2236:
2231:
2123:
2118:
2113:
2108:
2103:
2098:
2088:
2083:
2068:
2056:
2051:
2046:
2041:
2036:
2031:
2026:
2021:
2016:
2011:
2006:
1996:
1991:
1986:
1981:
1927:
1922:
1876:
1861:
1856:
1851:
1846:
1841:
1836:
1831:
1826:
1795:
1639:
1503:
1498:
447:
327:, as well as "point" sources, so named because they are smaller than the
233:
observations of the companion suggest that the mass of the pulsar is 2.7
1917:
1821:
1705:
1674:
1669:
1664:
1644:
1350:
1187:
435:
387:
212:
source, but was not recognized as a pulsar until observations with the
746:
Romani, R. W. (2012). "2FGL J1311.7-3429 Joins the Black Widow Club".
347:
sources, with the J1317.7–3429 designating its position in the sky in
2226:
1964:
1950:
1942:
1932:
1894:
1649:
1634:
1242:
443:
197:
179:
809:
760:
711:
654:
363:
495:
for neutron stars, strongly favoring "stiff" equations of state.
315:), the successor to EGRET, both performed surveys of the sky for
902:
849:
575:
616:"First black widow pulsar found from gamma ray observations"
331:
of the telescopes. Some point sources detected by EGRET and
295:, the previous record holder for most massive known pulsar.
442:
of this companion reveal that it is composed primarily of
339:, and included astrophysical sources such as pulsars and
200:
with a spin period of 2.5 milliseconds. It is the first
407:. The minimum mass found with this method is 8.2 x 10
470:
413:
270:
239:
2217:
2186:
2132:
1972:
1963:
1893:
1812:
1696:
1622:
1489:
1261:
1103:
1070:
910:
901:
225:, named after the original such system discovered,
576:"A black widow's Tango Mortale in gamma-ray light"
483:
426:
283:
252:
513:"Super-dense neutron star is fastest ever seen"
40:PSR J1311-3430 and its small stellar companion
861:
587:
585:
556:
554:
552:
550:
538:
536:
534:
532:
530:
403:mass of the companion to be determined using
8:
91:−34° 30′ 30.35″
2214:
2183:
1969:
1890:
1809:
1693:
907:
868:
854:
846:
808:
759:
710:
653:
475:
469:
418:
412:
275:
269:
244:
238:
51:J2000
305:Energetic Gamma Ray Experiment Telescope
206:Energetic Gamma Ray Experiment Telescope
503:
570:
568:
18:
7:
614:Francis, Matthew (25 October 2012).
291:, which is still more massive than
14:
434:, or roughly 8 times the mass of
2252:
2251:
591:
560:
542:
26:
309:Fermi Gamma-ray Space Telescope
214:Fermi Gamma-ray Space Telescope
1872:Scorpius–Centaurus association
893:Centaurus in Chinese astronomy
511:Wall, Mike (25 October 2012).
1:
602:
827:10.1088/2041-8205/760/2/L36
778:10.1088/2041-8205/754/2/L25
729:10.1088/2041-8205/763/1/L13
394:by material in the system.
2297:
888:List of stars in Centaurus
877:Constellation of Centaurus
484:{\displaystyle M_{\odot }}
427:{\displaystyle M_{\odot }}
299:Discovery and observations
284:{\displaystyle M_{\odot }}
253:{\displaystyle M_{\odot }}
2249:
2213:
2182:
1889:
1808:
1692:
883:
797:The Astrophysical Journal
748:The Astrophysical Journal
699:The Astrophysical Journal
172:
165:
158:
154:
115:
110:
95:
45:
24:
1208:V816 (Przybylski's Star)
672:10.1126/science.1229054
485:
428:
341:active galactic nuclei
285:
254:
578:. Max Planck Society.
543:Pletsch et al. (2012)
486:
429:
286:
255:
2201:Shapley Supercluster
1938:Southern Crab Nebula
1655:PSR B1259−63/LS 2883
935:C (Proxima Centauri)
561:Romani et al. (2012)
468:
411:
384:Green Bank Telescope
268:
237:
2276:Millisecond pulsars
2219:Astronomical events
925:A (Rigil Kentaurus)
819:2012ApJ...760L..36R
770:2012ApJ...754L..25R
721:2013ApJ...763L..13R
664:2012Sci...338.1314P
648:(6112): 1314–1317.
223:Black Widow Pulsars
173:Database references
21:
2094:5128 (Centaurus A)
1781:Proxima Centauri b
481:
424:
405:Kepler's third law
368:millisecond pulsar
329:angular resolution
281:
250:
202:millisecond pulsar
167:2FGL J1311.7–3429
160:Other designations
102:Spectral type
19:
2263:
2262:
2245:
2244:
2209:
2208:
2178:
2177:
1959:
1958:
1947:
1885:
1884:
1804:
1803:
1688:
1687:
1665:WASP-15 (Nyamien)
603:Ray et al. (2012)
493:equation of state
191:
190:
36:
2288:
2255:
2254:
2215:
2184:
1970:
1945:
1903:Boomerang Nebula
1891:
1810:
1694:
1680:WASP-167/KELT-13
1630:2MASS J1126−5003
908:
870:
863:
856:
847:
839:
838:
812:
790:
789:
763:
741:
740:
714:
692:
691:
657:
627:
626:
624:
622:
611:
605:
600:
594:
589:
580:
579:
572:
563:
558:
545:
540:
525:
524:
522:
520:
508:
490:
488:
487:
482:
480:
479:
433:
431:
430:
425:
423:
422:
307:(EGRET) and the
290:
288:
287:
282:
280:
279:
259:
257:
256:
251:
249:
248:
96:Characteristics
81:
76:
46:Observation data
38:
37:
22:
2296:
2295:
2291:
2290:
2289:
2287:
2286:
2285:
2266:
2265:
2264:
2259:
2241:
2205:
2188:Galaxy clusters
2174:
2160:IRAS 13224-3809
2128:
1955:
1881:
1800:
1684:
1618:
1584:117618 (Dofida)
1485:
1257:
1099:
1066:
897:
879:
874:
843:
794:
793:
745:
744:
696:
695:
639:
638:
635:
630:
620:
618:
613:
612:
608:
601:
597:
590:
583:
574:
573:
566:
559:
548:
541:
528:
518:
516:
510:
509:
505:
501:
471:
466:
465:
461:
414:
409:
408:
400:
398:Characteristics
349:right ascension
301:
271:
266:
265:
240:
235:
234:
168:
134:
131:
79:
74:Right ascension
72:
47:
41:
39:
27:
20:PSR J1311–3430
17:
12:
11:
5:
2294:
2292:
2284:
2283:
2278:
2268:
2267:
2261:
2260:
2250:
2247:
2246:
2243:
2242:
2240:
2239:
2234:
2229:
2223:
2221:
2211:
2210:
2207:
2206:
2204:
2203:
2198:
2192:
2190:
2180:
2179:
2176:
2175:
2173:
2172:
2167:
2162:
2157:
2152:
2147:
2142:
2136:
2134:
2130:
2129:
2127:
2126:
2121:
2116:
2111:
2106:
2101:
2096:
2091:
2086:
2081:
2076:
2071:
2066:
2065:
2064:
2054:
2049:
2044:
2039:
2034:
2029:
2024:
2019:
2014:
2009:
2004:
1999:
1994:
1989:
1984:
1978:
1976:
1967:
1961:
1960:
1957:
1956:
1954:
1953:
1948:
1940:
1935:
1930:
1925:
1920:
1915:
1910:
1905:
1899:
1897:
1887:
1886:
1883:
1882:
1880:
1879:
1874:
1869:
1864:
1859:
1854:
1849:
1844:
1839:
1834:
1829:
1824:
1818:
1816:
1806:
1805:
1802:
1801:
1799:
1798:
1793:
1788:
1783:
1778:
1773:
1768:
1763:
1758:
1753:
1748:
1743:
1738:
1733:
1728:
1723:
1718:
1713:
1708:
1702:
1700:
1690:
1689:
1686:
1685:
1683:
1682:
1677:
1672:
1667:
1662:
1660:PSR J1311–3430
1657:
1652:
1647:
1642:
1637:
1632:
1626:
1624:
1620:
1619:
1617:
1616:
1611:
1606:
1601:
1596:
1591:
1586:
1581:
1576:
1571:
1566:
1561:
1556:
1551:
1546:
1541:
1536:
1531:
1526:
1521:
1519:102117 (Uklun)
1516:
1511:
1506:
1501:
1495:
1493:
1487:
1486:
1484:
1483:
1478:
1473:
1468:
1463:
1458:
1453:
1448:
1443:
1438:
1433:
1428:
1423:
1418:
1413:
1408:
1403:
1398:
1393:
1388:
1383:
1378:
1373:
1368:
1363:
1358:
1353:
1348:
1343:
1338:
1333:
1328:
1323:
1318:
1313:
1308:
1303:
1298:
1293:
1288:
1283:
1278:
1273:
1267:
1265:
1259:
1258:
1256:
1255:
1250:
1245:
1240:
1235:
1230:
1225:
1220:
1215:
1210:
1205:
1200:
1195:
1190:
1185:
1180:
1175:
1170:
1165:
1160:
1155:
1150:
1145:
1140:
1135:
1130:
1125:
1120:
1115:
1109:
1107:
1101:
1100:
1098:
1097:
1092:
1087:
1082:
1076:
1074:
1068:
1067:
1065:
1064:
1059:
1054:
1049:
1044:
1039:
1034:
1029:
1024:
1019:
1014:
1009:
1004:
999:
994:
989:
984:
979:
974:
969:
964:
959:
954:
949:
944:
939:
938:
937:
932:
927:
916:
914:
905:
899:
898:
896:
895:
890:
884:
881:
880:
875:
873:
872:
865:
858:
850:
841:
840:
791:
754:(2): L25–L20.
742:
693:
634:
631:
629:
628:
606:
595:
581:
564:
546:
526:
502:
500:
497:
478:
474:
460:
457:
421:
417:
399:
396:
319:emission. The
300:
297:
293:PSR J1614−2230
278:
274:
247:
243:
194:PSR J1311–3430
189:
188:
183:
175:
174:
170:
169:
166:
163:
162:
156:
155:
152:
151:
145:
137:
136:
132:
129:
125:
117:
116:
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112:
108:
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104:
98:
97:
93:
92:
89:
83:
82:
77:
69:
68:
63:
57:
56:
43:
42:
25:
15:
13:
10:
9:
6:
4:
3:
2:
2293:
2282:
2279:
2277:
2274:
2273:
2271:
2258:
2248:
2238:
2235:
2233:
2230:
2228:
2225:
2224:
2222:
2220:
2216:
2212:
2202:
2199:
2197:
2194:
2193:
2191:
2189:
2185:
2181:
2171:
2168:
2166:
2163:
2161:
2158:
2156:
2153:
2151:
2148:
2146:
2143:
2141:
2138:
2137:
2135:
2131:
2125:
2122:
2120:
2117:
2115:
2112:
2110:
2107:
2105:
2102:
2100:
2097:
2095:
2092:
2090:
2087:
2085:
2082:
2080:
2077:
2075:
2072:
2070:
2067:
2063:
2060:
2059:
2058:
2055:
2053:
2050:
2048:
2045:
2043:
2040:
2038:
2035:
2033:
2030:
2028:
2025:
2023:
2020:
2018:
2015:
2013:
2010:
2008:
2005:
2003:
2000:
1998:
1995:
1993:
1990:
1988:
1985:
1983:
1980:
1979:
1977:
1975:
1971:
1968:
1966:
1962:
1952:
1949:
1944:
1941:
1939:
1936:
1934:
1931:
1929:
1926:
1924:
1921:
1919:
1916:
1914:
1911:
1909:
1906:
1904:
1901:
1900:
1898:
1896:
1892:
1888:
1878:
1875:
1873:
1870:
1868:
1865:
1863:
1860:
1858:
1855:
1853:
1850:
1848:
1845:
1843:
1840:
1838:
1835:
1833:
1830:
1828:
1825:
1823:
1820:
1819:
1817:
1815:
1814:Star clusters
1811:
1807:
1797:
1794:
1792:
1789:
1787:
1784:
1782:
1779:
1777:
1774:
1772:
1769:
1767:
1764:
1762:
1759:
1757:
1754:
1752:
1749:
1747:
1744:
1742:
1739:
1737:
1734:
1732:
1729:
1727:
1724:
1722:
1719:
1717:
1714:
1712:
1709:
1707:
1704:
1703:
1701:
1699:
1695:
1691:
1681:
1678:
1676:
1673:
1671:
1668:
1666:
1663:
1661:
1658:
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947:γ (Muhlifain)
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592:Romani (2012)
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374:wavelengths.
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231:Spectroscopic
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61:Constellation
59:
58:
54:
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44:
23:
2170:PKS 1353−341
2165:PKS 1144-379
2145:ESO 325-G004
1711:b Centauri b
1659:
842:
800:
796:
751:
747:
702:
698:
645:
641:
619:. Retrieved
609:
598:
517:. Retrieved
506:
462:
459:Significance
440:spectroscopy
401:
378:
376:
357:
344:
332:
312:
302:
262:solar masses
227:PSR B1957+20
208:as a bright
193:
192:
178:
140:
120:
80:13 11 45.724
1776:HIP 67522 b
1771:HIP 65426 b
1766:HD 121504 b
1761:HD 117618 b
1756:HD 117207 b
1751:HD 114729 b
1746:HD 114386 b
1736:HD 113538 b
1731:HD 101930 b
1726:HD 109749 b
1721:HD 103197 b
1716:HD 102117 b
972:θ (Menkent)
930:B (Toliman)
515:. Space.com
353:declination
337:wavelengths
87:Declination
2270:Categories
2196:Abell S740
2155:ESO 444-46
2150:ESO 383-76
2140:ESO 269-57
1913:G292.0+1.8
1698:Exoplanets
962:ζ (Alnair)
803:(2): L36.
705:(1): L13.
633:References
621:29 October
519:25 October
453:Roche lobe
446:, with no
438:. Optical
321:telescopes
2281:Centaurus
1908:Fleming 1
1072:Flamsteed
942:β (Hadar)
810:1210.6884
786:119262868
761:1207.1736
712:1210.6676
688:206544680
655:1211.1385
477:⊙
420:⊙
392:scattered
325:Milky Way
317:gamma ray
277:⊙
246:⊙
210:gamma ray
127:2.7
66:Centaurus
2257:Category
2237:SN 1986G
2232:SN 1895B
1965:Galaxies
1946:(RCW 86)
1928:NGC 5307
1923:NGC 3918
1877:Stock 16
1862:NGC 5662
1857:NGC 5617
1852:NGC 5460
1847:NGC 5316
1842:NGC 5281
1837:NGC 5286
1832:NGC 4230
1827:NGC 3766
1796:WASP-15b
1640:Gaia BH2
1481:5489 (c)
1476:5485 (c)
1471:5471 (b)
1461:5358 (v)
1441:5222 (y)
1436:5207 (N)
1431:5174 (z)
1426:5172 (M)
1421:5141 (Q)
1416:5089 (d)
1411:5071 (K)
1406:5041 (m)
1401:5035 (J)
1396:5006 (r)
1381:4940 (f)
1376:4889 (n)
1371:4888 (e)
1366:4874 (p)
1361:4831 (w)
1356:4817 (l)
1346:4748 (u)
1341:4732 (G)
1336:4724 (x)
1326:4712 (x)
1321:4682 (F)
1316:4652 (D)
1311:4620 (E)
1306:4546 (B)
1301:4537 (j)
1281:4476 (C)
1276:4466 (C)
1271:4460 (A)
1238:V945 (H)
1183:V763 (C)
1178:V761 (a)
1105:Variable
835:56207483
737:21255302
680:23112297
448:hydrogen
388:eclipsed
142:Rotation
133:☉
1918:IC 2944
1895:Nebulae
1822:IC 2944
1706:2M1207b
1675:WASP-42
1670:WASP-41
1645:GJ 3737
815:Bibcode
766:Bibcode
717:Bibcode
660:Bibcode
642:Science
436:Jupiter
360:optical
111:Details
106:Pulsar
53:Equinox
2227:SN 185
1951:SuWt 2
1943:SN 185
1933:RCW 79
1650:J1407b
1635:2M1207
1614:131399
1609:125595
1604:125072
1599:124448
1594:121504
1589:121228
1579:117207
1574:116434
1569:115600
1564:114729
1559:114386
1554:113766
1549:113538
1544:110113
1539:109749
1534:108236
1529:107914
1524:103197
1514:101930
1509:100453
833:
784:
735:
686:
678:
444:helium
218:period
198:pulsar
180:SIMBAD
55:J2000
16:Pulsar
2133:Other
2002:4650A
1623:Other
1504:98176
1499:97413
1253:V1400
1248:V1369
1243:V1032
1095:4 (h)
1090:3 (k)
1085:2 (g)
1080:1 (i)
912:Bayer
903:Stars
831:S2CID
805:arXiv
782:S2CID
756:arXiv
733:S2CID
707:arXiv
684:S2CID
650:arXiv
499:Notes
379:Fermi
372:radio
364:X-ray
345:Fermi
333:Fermi
313:Fermi
196:is a
49:Epoch
2124:5419
2119:5408
2114:5398
2109:5291
2104:5253
2099:5161
2089:5114
2084:5102
2079:5091
2074:5090
2069:5026
2057:5011
2052:4976
2047:4945
2042:4744
2037:4743
2032:4730
2027:4729
2022:4709
2017:4706
2012:4696
2007:4683
1997:4622
1992:4603
1987:4444
1982:3783
1466:5371
1456:5297
1451:5241
1446:5224
1391:4989
1386:4979
1351:4796
1331:4721
1296:4523
1291:4522
1286:4499
1233:V863
1228:V886
1223:V885
1218:V842
1213:V831
1203:V810
1198:V803
1193:V779
1188:V766
1173:V752
1168:V744
1163:V346
676:PMID
623:2012
521:2012
362:and
351:and
303:The
186:data
147:2.5
122:Mass
1974:NGC
823:doi
801:760
774:doi
752:754
725:doi
703:763
668:doi
646:338
390:or
355:).
2272::
1491:HD
1263:HR
1158:DY
1153:BV
1148:SX
1143:SV
1138:RR
829:.
821:.
813:.
799:.
780:.
772:.
764:.
750:.
731:.
723:.
715:.
701:.
682:.
674:.
666:.
658:.
644:.
584:^
567:^
549:^
529:^
149:ms
2062:A
1867:ω
1791:d
1786:c
1741:c
1133:Y
1128:V
1123:U
1118:T
1113:R
1062:ψ
1057:χ
1052:φ
1047:υ
1042:υ
1037:τ
1032:σ
1027:ρ
1022:π
1017:ο
1012:ο
1007:ξ
1002:ξ
997:ν
992:μ
987:λ
982:κ
977:ι
967:η
957:ε
952:δ
920:α
869:e
862:t
855:v
837:.
825::
817::
807::
788:.
776::
768::
758::
739:.
727::
719::
709::
690:.
670::
662::
652::
625:.
523:.
473:M
416:M
311:(
273:M
260:(
242:M
130:M
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