50:
629:
694:
and exceptional long minimum, longer even than a deep five year minimum which had occurred in 1962ā7. It then faded again to near 15th magnitude, and by August 2014 it had been below 10th magnitude for 7 years. In late 2014, it brightened quickly to 7th magnitude but then began to fade again. By mid-2017, it had been below its "normal" brightness for ten years. It also reached a new record faintest at magnitude 15.2.
779:
57:
1090:
Cutri, Roc M.; Skrutskie, Michael F.; Van Dyk, Schuyler D.; Beichman, Charles A.; Carpenter, John M.; Chester, Thomas; Cambresy, Laurent; Evans, Tracey E.; Fowler, John W.; Gizis, John E.; Howard, Elizabeth V.; Huchra, John P.; Jarrett, Thomas H.; Kopan, Eugene L.; Kirkpatrick, J. Davy; Light, Robert
693:
In August 2007, R Coronae
Borealis began a fade to an unprecedented minimum. It fell to 14th magnitude in 33 days, then continued to fade slowly, dropping below 15th magnitude in June 2009. It then began an equally slow rise, not reaching 12th magnitude until late 2011. This was an unusually deep
661:
At irregular intervals a few years or decades apart R Coronae
Borealis fades from its normal brightness near 6th magnitude for a period of months or sometimes years. There is no fixed minimum, but the star can become fainter than 15th magnitude in the visual range. The fading is less pronounced at
1757:
Clayton, Geoffrey C.; Sugerman, Ben E. K.; Adam
Stanford, S.; Whitney, B. A.; Honor, J.; Babler, B.; Barlow, M. J.; Gordon, K. D.; Andrews, J. E.; Geballe, T. R.; Bond, Howard E.; De Marco, O.; Lawson, W. A.; Sibthorpe, B.; Olofsson, G.; Polehampton, E.; Gomez, H. L.; Matsuura, M.; Hargrave, P. C.;
651:. Much of the time it shows variations of around a tenth of a magnitude with poorly defined periods that have been reported as 40 and 51 days. These correspond to the first overtone and fundamental radial pulsation modes for an extreme helium star slightly under one
761:
The spectrum at maximum indicates that hydrogen in R Coronae
Borealis is strongly depleted, helium is the dominant element, and carbon is strongly enhanced. At minimum, the spectrum shows the development of carbon clouds that obscure the
666:. Typically the star starts to return to maximum brightness almost immediately from its minimum, although occasionally this is interrupted by another fade. The cause of this behaviour is believed to be a regular build-up of
1923:
Jeffers, S. V.; Min, M.; Waters, L. B. F. M.; Canovas, H.; Rodenhuis, M.; De Juan Ovelar, M.; Chies-Santos, A. L.; Keller, C. U. (2012). "Direct imaging of a massive dust cloud around R Coronae
Borealis".
581:, but at intervals of several months to many years fades to as faint as 15th magnitude. Over successive months it then gradually returns to its normal brightness, giving it the nickname "reverse
647:
R Coronae
Borealis is the prototype of the R Coronae Borealis class of variable stars. It is one of only two R Coronae Borealis variables bright enough to be seen with the naked eye, along with
899:, and coarser dust (composed of grains with a diameter of around 0.14 Ī¼m) ejected periodically. The obscuration appears to happen closer to the star as clouds of carbon condense at
1091:
M.; Marsh, Kenneth A.; McCallon, Howard L.; Schneider, Stephen E.; Stiening, Rae; Sykes, Matthew J.; Weinberg, Martin D.; Wheaton, William A.; Wheelock, Sherry L.; Zacarias, N. (2003).
1758:
Ivison, R. J.; Wesson, R.; Leeks, S. J.; Swinyard, B. M.; Lim, T. L. (2011). "The
Circumstellar Environment of R Coronae Borealis: White Dwarf Merger or Final-Helium-Shell Flash?".
876:
in the atmosphere is not easily explained by the merger model, but is a natural consequence of a late helium flash. Evolutionary models of post-AGB stars give a mass of 0.66
485:
525:
2568:
605:
numbered all the Bayer stars but did not add any additional designations for fainter stars, so R Coronae
Borealis does not appear in either of these two catalogues.
418:
758:. In deep minima, many of the metal lines disappear although the Ca doublet remains strong. Forbidden "nebular" lines of , , and can be detected at times.
2008:
786:
R Coronae
Borealis is about 90% helium and less than 1% hydrogen. The majority of the remainder is carbon. This classifies it as a carbon-enhanced
2038:
812:
The distance of R Coronae
Borealis is not known exactly, but is estimated at 1.4 kiloparsecs from assumptions about its intrinsic brightness. The
2553:
2573:
686:, resulting in much of the star's light being blocked. The gradual restoration to normal brightness results from the dust being dispersed by
2563:
895:
from R Coronae Borealis, corresponding to a stream of fine dust (composed of grains about 5 nm in diameter) associated with the star's
2033:
1432:"On the Periodical Changes of Brightness of Two Fixed Stars. By Edward Pigott, Esq. Communicated by Sir Henry C. Englefield, Bart. F. R. S"
1259:
Montiel, Edward J.; Clayton, Geoffrey C.; Marcello, Dominic C.; Lockman, Felix J. (2015). "What is the Shell Around R Coronae Borealis?".
1001:
Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)".
1145:
White, Russel J.; Gabor, Jared M.; Hillenbrand, Lynne A. (2007). "High-Dispersion Optical Spectra of Nearby Stars Younger Than the Sun".
945:
Gaia Collaboration; et al. (November 2016). "Gaia Data Release 1. Summary of the astrometric, photometric, and survey properties".
1504:
469:
872:
so it is thought to have formed by the merger of a carbon-oxygen white dwarf and a helium white dwarf. The detection of significant
1813:"Post-merger evolution of carbon-oxygen + helium white dwarf binaries and the origin of R Coronae Borealis and extreme helium stars"
865:
in a post-AGB star. Models of post-AGB stars calculate that a star with the appearance of R CrB would have a mass around 0.6
612:, "Variable (star) of Corona (Borealis)". It has also been called a "reverse nova" because of its habit of fading from sight. The
2028:
2593:
2583:
78:
1870:
StasiÅska, G.; Szczerba, R.; Schmidt, M.; SiĆ³dmiak, N. (2006). "Post-AGB stars as testbeds of nucleosynthesis in AGB stars".
1398:
Asplund, M.; Gustafsson, B.; Lambert, D. L.; Rao, N. K. (2000). "The R Coronae Borealis stars - atmospheres and abundances".
1345:
Clayton, Geoffrey C.; Geballe, T. R.; Zhang, Wanshu (2013). "Variable Winds and Dust Formation in R Coronae Borealis Stars".
577:
at irregular intervals. R Coronae Borealis itself normally shines at approximately magnitude 6, just about visible to the
2001:
617:
2578:
566:
210:
20:
2588:
2353:
2343:
820:
whose distances are known quite accurately. The luminosity is estimated from helium star models to be 19,000
1060:
Ducati, J. R. (2002). "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system".
2200:
613:
457:
2558:
2348:
2170:
2145:
2085:
1994:
1602:
Skuljan, L.; Cottrell, P. L. (2002). "Recent declines of RS Telescopii, UW Centauri, and V Coronae Australis".
910:
from the surface, and are visible as cometary knots when they lie to side of the star. There is also a 2
841:
There is a fainter star 3" away from R Coronae Borealis, but it is believed to be a distant class K dwarf. Its
608:
At its discovery it was described simply as "the variable in the Northern crown". It was later referred to as
1122:
Mattei, Janet A.; Waagen, Elizabeth O.; Foster, E. Grant (1991). "R Coronae Borealis light curves 1843-1990".
754:, and other metals. The lines are typically very narrow at this stage. Helium emission lines sometimes show
2120:
2598:
2373:
2368:
2363:
2358:
2263:
2160:
2115:
2105:
2080:
2075:
2065:
891:
Direct imaging with the Hubble Space Telescope shows extensive dust clouds out to a radius of around 2000
817:
497:
481:
140:
2420:
2180:
2110:
2095:
2090:
2070:
513:
461:
426:
838:
data release 1 parallax also gives a distance of 1.4 kpc although with a considerable margin of error.
546:
640:
in 1795. In 1935 it was the first star shown to have a different chemical composition to the Sun via
49:
2165:
2155:
2135:
2130:
2100:
1943:
1889:
1834:
1777:
1726:
1681:
1641:
1611:
1576:
1529:
1443:
1407:
1364:
1324:
1278:
1220:
1164:
1127:
1104:
1069:
1037:
1010:
964:
301:
31:
734:
are also present. The spectrum is variable, most obviously during the brightness fades. The normal
2253:
2248:
2243:
2238:
2150:
2140:
2125:
787:
735:
501:
27:
628:
2233:
2228:
2223:
2218:
2213:
1959:
1933:
1905:
1879:
1852:
1824:
1793:
1767:
1699:
1469:
1461:
1380:
1354:
1294:
1268:
1236:
1210:
1180:
1154:
980:
954:
846:
813:
791:
687:
671:
574:
493:
473:
316:
123:
1634:
The Society for Astronomical Sciences 25th Annual Symposium on Telescope Science. Held May 23ā25
903:
regions in an expanding front. "Puffs" of dust emitted from the star condense at about 85
2335:
2057:
1500:
1496:
1489:
892:
835:
805:
at maximum is reasonably well known at 6,900K and appears to decrease during the fades as the
598:
74:
2528:
1951:
1947:
1897:
1893:
1842:
1785:
1734:
1689:
1584:
1451:
1411:
1372:
1286:
1228:
1224:
1172:
972:
968:
918:
703:
393:
285:
1092:
632:
Light curve of R Coronae Borealis from 1990 to 2017, showing the unprecedented deep minimum
585:", after the more common type of star which rapidly increases in brightness before fading.
2464:
2017:
1567:
Berman, Louis (1935). "The Spectrum Analysis of the Hot Carbon Star, R Coronae Borealis".
755:
562:
489:
453:
406:
229:
99:
91:
1838:
1781:
1730:
1685:
1645:
1615:
1580:
1533:
1447:
1368:
1328:
1282:
1168:
1131:
1108:
1073:
1041:
1014:
2488:
602:
593:
R Coronae Borealis is a faint naked eye star, but does not have any traditional names.
477:
444:
293:
273:
257:
2547:
1856:
1797:
1789:
1703:
1473:
1384:
1376:
1298:
1290:
739:
648:
637:
570:
246:
205:
86:
1963:
1909:
1240:
1986:
984:
896:
862:
767:
675:
641:
594:
373:
346:
1955:
1184:
1093:"VizieR Online Data Catalog: 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)"
976:
778:
1901:
1548:
1232:
1003:
VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S
2189:
900:
858:
842:
806:
802:
763:
195:
184:
173:
162:
151:
112:
2523:
2518:
2513:
2508:
2503:
2297:
857:
There are two main models for the formation of R CrB stars: the merger of two
663:
558:
386:
353:
217:
2389:
2326:
2276:
2271:
1847:
1812:
578:
1456:
1315:
Saio, H. (2008). "Radial and Nonradial Pulsations in RCB and EHe-B Stars".
636:
The variability of R Coronae Borealis was discovered by English astronomer
849:
are not consistent with being at the same distance as R Coronae Borealis.
2448:
2443:
2438:
2433:
2428:
2307:
2292:
1884:
715:
707:
2474:
2469:
2302:
1717:
Searle, Leonard (1961). "An Abundance Analysis of R Coronae Borealis".
873:
731:
1465:
706:
a late F or early G yellow supergiant, but with marked peculiarities.
2411:
1632:
Watson, C. L. (2006). "The International Variable Star Index (VSX)".
1201:
Van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction".
917:
shell about 4 pc wide containing dust at 25 K, which may be a fossil
723:
711:
679:
667:
540:
433:
366:
308:
1431:
1738:
1694:
1669:
1588:
1273:
1176:
959:
2397:
1980:
1938:
1829:
1772:
1670:"Optical Spectroscopy at Deep Light Minimum of R Coronae Borealis"
1359:
1215:
1159:
777:
727:
627:
517:
505:
465:
56:
2312:
2048:
683:
582:
521:
509:
277:
261:
1990:
1028:
Klochkova, V. G. (1997). "Supergiants with large IR excesses".
816:
of ā5 is calculated by comparison with R CrB variables in the
1668:
Howell, Steve B.; Rector, Travis A.; Walter, Donald (2013).
674:. The sudden drop in brightness may be caused by a rapid
1436:
Philosophical Transactions of the Royal Society of London
1674:
Publications of the Astronomical Society of the Pacific
19:
This article is about the star. For the star type, see
1811:
Zhang, X.; Jeffery, C. S.; Chen, X.; Han, Z. (2014).
616:
R Coronae Borealis was introduced, as "Coronae R" by
883:
for R CrB, but with a considerable margin of error.
2496:
2487:
2457:
2419:
2410:
2382:
2334:
2325:
2285:
2262:
2199:
2179:
2056:
2047:
1520:Bone, Neil (2006). "Skky notes for April and May".
1488:
16:Variable star in the constellation Corona Borealis
1817:Monthly Notices of the Royal Astronomical Society
1030:Bulletin of the Special Astrophysical Observatory
1522:Journal of the British Astronomical Association
1340:
1338:
1317:Hydrogen-Deficient Stars ASP Conference Series
794:suggests that the star's mass is 0.8-0.9
702:R Coronae Borealis at maximum light shows the
601:designation although it is marked on his map.
2002:
1430:Pigott, Edward; Englefield, Henry C. (1797).
8:
117:+28° 09′ 24.295″
1196:
1194:
1097:CDS/ADC Collection of Electronic Catalogues
1062:CDS/ADC Collection of Electronic Catalogues
77:J2000.0
2493:
2416:
2331:
2053:
2009:
1995:
1987:
1752:
1750:
1748:
827:and the star has a radius around 100
1937:
1883:
1846:
1828:
1771:
1693:
1663:
1661:
1659:
1657:
1655:
1562:
1560:
1455:
1425:
1423:
1421:
1358:
1272:
1254:
1252:
1250:
1214:
1158:
958:
1055:
1053:
1051:
66:Location of R Coronae Borealis (circled)
2569:Objects with variable star designations
1550:Humboldts Kosmos: In verkĆ¼rzter Gestalt
1310:
1308:
1085:
1083:
930:
253:
1627:
1625:
996:
994:
36:
940:
938:
936:
934:
7:
2034:Corona Borealis in Chinese astronomy
2039:HerculesāCorona Borealis Great Wall
1495:. Dover Publications, Inc. p.
782:R Coronae Borealis in optical light
265:
1491:Star Names: Their Lore and Meaning
14:
1981:AAVSO Variable Star of the Season
492: 2039-1605-1, CDS 886,
2029:List of stars in Corona Borealis
2018:Constellation of Corona Borealis
809:is obscured by condensing dust.
710:lines are weak or absent, while
55:
48:
1547:Alexander von Humboldt (1850).
2554:Henry Draper Catalogue objects
1442:. The Royal Society: 133ā141.
565:. It is the prototype of the
1:
2574:Bright Star Catalogue objects
714:lines and molecular bands of
561:star in the constellation of
2564:R Coronae Borealis variables
1926:Astronomy & Astrophysics
947:Astronomy & Astrophysics
618:Friedrich Wilhelm Argelander
1956:10.1051/0004-6361/201117138
977:10.1051/0004-6361/201629512
722:are exceptionally strong.
567:R Coronae Borealis variable
292:0.73 Ā± 0.27
21:R Coronae Borealis variable
2615:
1902:10.1051/0004-6361:20053553
1872:Astronomy and Astrophysics
1790:10.1088/0004-637X/743/1/44
1400:Astronomy and Astrophysics
1377:10.1088/0004-6256/146/2/23
1291:10.1088/0004-6256/150/1/14
1233:10.1051/0004-6361:20078357
1203:Astronomy and Astrophysics
25:
18:
2024:
1760:The Astrophysical Journal
1569:The Astrophysical Journal
614:variable star designation
533:
468: J15483440+2809242,
450:
443:
439:
340:
335:
331:
223:
216:
134:
71:
42:
1347:The Astronomical Journal
1261:The Astronomical Journal
1147:The Astronomical Journal
770:lines visible at times.
573:, which fade by several
26:Not to be confused with
1948:2012A&A...539A..56J
1894:2006A&A...450..701S
1553:. Greiner und Pfeiffer.
1412:2000A&A...353..287A
1225:2007A&A...474..653V
969:2016A&A...595A...2G
317:Absolute magnitude
124:Apparent magnitude
2594:IRAS catalogue objects
2584:Durchmusterung objects
1457:10.1098/rstl.1797.0007
887:Circumstellar material
818:Large Magellanic Cloud
783:
682:-rich dust similar to
633:
1848:10.1093/mnras/stu1741
1719:Astrophysical Journal
1487:Allen, R. H. (1963).
781:
631:
557:is a low-mass yellow
2359:Ļ Coronae Borealis b
2354:Īæ Coronae Borealis b
2349:Īŗ Coronae Borealis b
2344:Īµ Coronae Borealis b
32:Rho Coronae Borealis
1839:2014MNRAS.445..660Z
1782:2011ApJ...743...44C
1731:1961ApJ...133..531S
1686:2013PASP..125..879H
1646:2006SASS...25...47W
1616:2002Obs...122..322S
1581:1935ApJ....81..369B
1534:2006JBAA..116..102B
1448:1797RSPT...87..133P
1369:2013AJ....146...23C
1329:2008ASPC..391...69S
1283:2015AJ....150...14M
1169:2007AJ....133.2524W
1132:1991rcbl.book.....M
1109:2003yCat.2246....0C
1074:2002yCat.2237....0D
1042:1997BSAO...44....5K
1015:2009yCat....102025S
788:extreme helium star
736:absorption spectrum
670:dust in the star's
534:Database references
476: 02039-01605,
464: N1330022410,
39:
38:R Coronae Borealis
28:RR Coronae Borealis
2579:G-type supergiants
893:astronomical units
847:apparent magnitude
814:absolute magnitude
784:
688:radiation pressure
634:
610:Variabilis Coronae
597:did not give it a
555:R Coronae Borealis
524: 15465+2818,
445:Other designations
206:Variable type
141:Spectral type
37:
2589:Hipparcos objects
2541:
2540:
2537:
2536:
2483:
2482:
2406:
2405:
2321:
2320:
2313:XO-1 (Moldoveanu)
861:; or a very late
642:spectral analysis
552:
551:
256: -2.10
2606:
2494:
2417:
2332:
2054:
2011:
2004:
1997:
1988:
1968:
1967:
1941:
1920:
1914:
1913:
1887:
1885:astro-ph/0601504
1867:
1861:
1860:
1850:
1832:
1808:
1802:
1801:
1775:
1754:
1743:
1742:
1714:
1708:
1707:
1697:
1680:(930): 879ā888.
1665:
1650:
1649:
1629:
1620:
1619:
1599:
1593:
1592:
1564:
1555:
1554:
1544:
1538:
1537:
1517:
1511:
1510:
1494:
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1478:
1477:
1459:
1427:
1416:
1415:
1395:
1389:
1388:
1362:
1342:
1333:
1332:
1312:
1303:
1302:
1276:
1256:
1245:
1244:
1218:
1198:
1189:
1188:
1162:
1153:(6): 2524ā2536.
1142:
1136:
1135:
1119:
1113:
1112:
1087:
1078:
1077:
1057:
1046:
1045:
1025:
1019:
1018:
998:
989:
988:
962:
942:
919:planetary nebula
790:. Modelling the
756:P Cygni profiles
520: 1544+28A,
480:+28Ā° 2477,
472:+28Ā° 1513,
454:Coronae Borealis
271:
267:
255:
135:Characteristics
127:
107:
102:
72:Observation data
59:
52:
40:
2614:
2613:
2609:
2608:
2607:
2605:
2604:
2603:
2559:Corona Borealis
2544:
2543:
2542:
2533:
2529:RX J1532.9+3021
2489:Galaxy clusters
2479:
2453:
2402:
2378:
2317:
2281:
2258:
2195:
2175:
2043:
2020:
2015:
1977:
1972:
1971:
1922:
1921:
1917:
1869:
1868:
1864:
1810:
1809:
1805:
1756:
1755:
1746:
1716:
1715:
1711:
1667:
1666:
1653:
1631:
1630:
1623:
1604:The Observatory
1601:
1600:
1596:
1566:
1565:
1558:
1546:
1545:
1541:
1519:
1518:
1514:
1507:
1486:
1485:
1481:
1429:
1428:
1419:
1397:
1396:
1392:
1344:
1343:
1336:
1314:
1313:
1306:
1258:
1257:
1248:
1200:
1199:
1192:
1144:
1143:
1139:
1124:AAVSO Monograph
1121:
1120:
1116:
1089:
1088:
1081:
1059:
1058:
1049:
1027:
1026:
1022:
1000:
999:
992:
944:
943:
932:
927:
916:
913:
909:
906:
889:
882:
879:
871:
868:
855:
833:
830:
826:
823:
800:
797:
776:
753:
749:
745:
742:, especially He
738:is replaced by
721:
700:
657:
654:
626:
591:
563:Corona Borealis
529:
407:Surface gravity
399:
396:
379:
376:
359:
356:
322:
269:
264:
240:27.83 km/s
235:
230:Radial velocity
122:
105:
100:Right ascension
98:
92:Corona Borealis
73:
67:
65:
64:
63:
62:
61:
60:
35:
24:
17:
12:
11:
5:
2612:
2610:
2602:
2601:
2596:
2591:
2586:
2581:
2576:
2571:
2566:
2561:
2556:
2546:
2545:
2539:
2538:
2535:
2534:
2532:
2531:
2526:
2521:
2516:
2511:
2506:
2500:
2498:
2491:
2485:
2484:
2481:
2480:
2478:
2477:
2472:
2467:
2465:FSC 15307+3253
2461:
2459:
2455:
2454:
2452:
2451:
2446:
2441:
2436:
2431:
2425:
2423:
2414:
2408:
2407:
2404:
2403:
2401:
2400:
2398:XO-1b (Negoiu)
2395:
2392:
2386:
2384:
2380:
2379:
2377:
2376:
2371:
2366:
2361:
2356:
2351:
2346:
2340:
2338:
2329:
2323:
2322:
2319:
2318:
2316:
2315:
2310:
2305:
2300:
2295:
2289:
2287:
2283:
2282:
2280:
2279:
2277:145457 (Kamuy)
2274:
2268:
2266:
2260:
2259:
2257:
2256:
2251:
2246:
2241:
2236:
2231:
2226:
2221:
2216:
2211:
2205:
2203:
2197:
2196:
2194:
2193:
2185:
2183:
2177:
2176:
2174:
2173:
2168:
2163:
2158:
2153:
2148:
2143:
2138:
2133:
2128:
2123:
2118:
2113:
2108:
2103:
2098:
2093:
2088:
2083:
2078:
2073:
2068:
2062:
2060:
2051:
2045:
2044:
2042:
2041:
2036:
2031:
2025:
2022:
2021:
2016:
2014:
2013:
2006:
1999:
1991:
1985:
1984:
1983:, January 2000
1976:
1975:External links
1973:
1970:
1969:
1915:
1862:
1823:(1): 660ā673.
1803:
1744:
1739:10.1086/147056
1709:
1695:10.1086/672163
1651:
1621:
1594:
1589:10.1086/143644
1556:
1539:
1512:
1506:978-0486210797
1505:
1479:
1417:
1390:
1334:
1304:
1246:
1209:(2): 653ā664.
1190:
1177:10.1086/514336
1137:
1114:
1079:
1047:
1020:
990:
929:
928:
926:
923:
914:
911:
907:
904:
888:
885:
880:
877:
869:
866:
854:
851:
831:
828:
824:
821:
798:
795:
775:
772:
751:
747:
743:
740:emission lines
719:
699:
696:
655:
652:
625:
622:
603:John Flamsteed
590:
587:
571:variable stars
550:
549:
544:
536:
535:
531:
530:
496: 104338,
484: 141527,
451:
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69:
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54:
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47:
46:
45:
44:
43:
15:
13:
10:
9:
6:
4:
3:
2:
2611:
2600:
2599:2MASS objects
2597:
2595:
2592:
2590:
2587:
2585:
2582:
2580:
2577:
2575:
2572:
2570:
2567:
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2255:
2252:
2250:
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2245:
2242:
2240:
2237:
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2232:
2230:
2227:
2225:
2222:
2220:
2217:
2215:
2212:
2210:
2207:
2206:
2204:
2202:
2198:
2192:
2191:
2187:
2186:
2184:
2182:
2178:
2172:
2169:
2167:
2164:
2162:
2159:
2157:
2154:
2152:
2149:
2147:
2144:
2142:
2139:
2137:
2134:
2132:
2129:
2127:
2124:
2122:
2119:
2117:
2114:
2112:
2109:
2107:
2104:
2102:
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2094:
2092:
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2027:
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2019:
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2000:
1998:
1993:
1992:
1989:
1982:
1979:
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1974:
1965:
1961:
1957:
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1935:
1931:
1927:
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1916:
1911:
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1877:
1873:
1866:
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1831:
1826:
1822:
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1807:
1804:
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1300:
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1204:
1197:
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1063:
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1048:
1043:
1039:
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1021:
1016:
1012:
1008:
1004:
997:
995:
991:
986:
982:
978:
974:
970:
966:
961:
956:
952:
948:
941:
939:
937:
935:
931:
924:
922:
920:
902:
898:
894:
886:
884:
875:
864:
860:
852:
850:
848:
844:
839:
837:
819:
815:
810:
808:
804:
793:
789:
780:
773:
771:
769:
768:chromospheric
765:
759:
757:
741:
737:
733:
729:
725:
717:
713:
709:
705:
697:
695:
691:
689:
685:
681:
677:
673:
669:
665:
659:
650:
649:RY Sagittarii
645:
643:
639:
638:Edward Pigott
630:
623:
621:
619:
615:
611:
606:
604:
600:
596:
588:
586:
584:
580:
576:
572:
568:
564:
560:
556:
548:
545:
543:
542:
538:
537:
532:
528: 84015.
527:
523:
519:
515:
511:
507:
504: 77442,
503:
500: 21257,
499:
495:
491:
488: 3581,
487:
483:
479:
475:
471:
467:
463:
459:
455:
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446:
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438:
435:
431:
429:
428:
424:
423:
420:
416:
414:
412:
408:
404:
403:
400:
392:~10,000
391:
389:
388:
384:
383:
380:
371:
369:
368:
364:
363:
360:
352:0.8-0.9
351:
349:
348:
344:
343:
339:
334:
330:
326:
324:
318:
314:
313:
310:
306:
304:
303:
299:
298:
295:
291:
289:
287:
283:
282:
279:
275:
263:
259:
252:
250:
248:
247:Proper motion
244:
243:
239:
237:
231:
227:
226:
222:
219:
215:
212:
209:
207:
204:
203:
199:
197:
193:
192:
188:
186:
182:
181:
177:
175:
171:
170:
166:
164:
160:
159:
155:
153:
149:
148:
144:
142:
139:
138:
133:
129:
125:
121:
120:
116:
114:
111:
110:
106:15 48 34.4147
104:
101:
97:
96:
93:
90:
88:
87:Constellation
85:
84:
80:
76:
70:
58:
51:
41:
33:
29:
22:
2208:
2188:
2066:Ī± (Alphecca)
1932:(A56): A56.
1929:
1925:
1918:
1875:
1871:
1865:
1820:
1816:
1806:
1763:
1759:
1722:
1718:
1712:
1677:
1673:
1637:
1633:
1607:
1603:
1597:
1572:
1568:
1549:
1542:
1525:
1521:
1515:
1490:
1482:
1439:
1435:
1403:
1399:
1393:
1350:
1346:
1320:
1316:
1264:
1260:
1206:
1202:
1150:
1146:
1140:
1123:
1117:
1100:
1096:
1065:
1061:
1033:
1029:
1023:
1006:
1002:
950:
946:
897:stellar wind
890:
863:helium flash
859:white dwarfs
856:
840:
811:
785:
760:
701:
692:
676:condensation
660:
646:
635:
609:
607:
599:Greek letter
595:Johann Bayer
592:
589:Nomenclature
554:
553:
539:
516: 5880,
512: 9116,
508: 4219,
425:
410:
405:
385:
365:
345:
315:
300:
284:
245:
228:
130:5.71 - 14.8
2071:Ī² (Nusakan)
807:photosphere
803:temperature
764:photosphere
664:wavelengths
624:Variability
460: CrB,
432:6,750
427:Temperature
307:1,400
196:color index
185:color index
174:color index
163:color index
152:color index
113:Declination
2548:Categories
2327:Exoplanets
2298:Gliese 611
1878:(2): 701.
1528:(2): 102.
1274:1505.04173
1103:: II/246.
960:1609.04172
925:References
792:pulsations
774:Properties
766:, leaving
726:lines and
718:(CN) and C
672:atmosphere
575:magnitudes
559:supergiant
409:(log
387:Luminosity
218:Astrometry
2390:GJ 3929 b
2181:Flamsteed
1939:1203.1265
1857:118506564
1830:1408.5500
1798:119240518
1773:1110.3235
1766:(1): 44.
1704:120129277
1474:186214528
1385:118385818
1360:1305.5047
1353:(2): 23.
1299:119271048
1267:(1): 14.
1216:0708.1752
1160:0706.0542
853:Formation
620:in 1850.
579:naked eye
417:0.5
126: (V)
2412:Galaxies
2308:NGC 6002
2293:ADS 9731
2201:Variable
1964:55589182
1910:12040452
1241:18759600
915:☉
908:☉
881:☉
870:☉
832:☉
825:☉
799:☉
730:such as
716:cyanogen
708:Hydrogen
704:spectrum
698:Spectrum
656:☉
398:☉
378:☉
372:85
358:☉
319: (M
302:Distance
286:Parallax
81:J2000.0
2475:IC 4539
2470:IC 1166
2303:GJ 3929
1944:Bibcode
1890:Bibcode
1835:Bibcode
1778:Bibcode
1727:Bibcode
1725:: 531.
1682:Bibcode
1642:Bibcode
1612:Bibcode
1610:: 322.
1577:Bibcode
1575:: 369.
1530:Bibcode
1444:Bibcode
1408:Bibcode
1406:: 287.
1365:Bibcode
1325:Bibcode
1279:Bibcode
1221:Bibcode
1165:Bibcode
1128:Bibcode
1105:Bibcode
1070:Bibcode
1038:Bibcode
1011:Bibcode
985:1828208
965:Bibcode
874:lithium
834:. The
801:. The
732:calcium
662:longer
452:R
336:Details
79:Equinox
2272:140913
2190:23 Her
1962:
1908:
1855:
1796:
1702:
1640:: 47.
1503:
1472:
1466:106921
1464:
1383:
1323:: 69.
1297:
1239:
1185:122854
1183:
983:
953:: 23.
843:colour
728:metals
724:Helium
712:carbon
680:carbon
668:carbon
541:SIMBAD
367:Radius
272:
270:ā11.52
268:
200:0.800
189:0.275
145:G0Iep
2497:Abell
2458:Other
2383:Other
2336:Bayer
2286:Other
2058:Bayer
2049:Stars
1960:S2CID
1934:arXiv
1906:S2CID
1880:arXiv
1853:S2CID
1825:arXiv
1794:S2CID
1768:arXiv
1700:S2CID
1470:S2CID
1462:JSTOR
1381:S2CID
1355:arXiv
1295:S2CID
1269:arXiv
1237:S2CID
1211:arXiv
1181:S2CID
1155:arXiv
1068:: 0.
1036:: 5.
987:. A2.
981:S2CID
955:arXiv
901:shock
518:AAVSO
506:RAFGL
466:2MASS
266:Dec.:
211:R CrB
178:0.45
167:0.60
156:0.13
75:Epoch
2524:2162
2519:2142
2514:2067
2509:2065
2504:2061
2449:6122
2444:6120
2439:6104
2434:6086
2429:6085
1501:ISBN
1101:2246
1066:2237
845:and
836:Gaia
750:, Na
746:, Ca
684:soot
583:nova
547:data
522:IRAS
510:GCRV
462:GSC2
347:Mass
194:JāK
183:JāH
172:VāR
161:BāV
150:UāB
2421:NGC
1952:doi
1930:539
1898:doi
1876:450
1843:doi
1821:445
1786:doi
1764:743
1735:doi
1723:133
1690:doi
1678:125
1608:122
1585:doi
1526:116
1497:178
1452:doi
1404:353
1373:doi
1351:146
1321:391
1287:doi
1265:150
1229:doi
1207:474
1173:doi
1151:133
973:doi
951:595
678:of
569:of
526:SAO
502:HIP
494:PPM
490:TYC
486:PLX
474:GSC
419:cgs
294:mas
288:(Ļ)
274:mas
258:mas
254:RA:
249:(Ī¼)
30:or
2550::
2264:HD
2254:UW
2249:TY
2244:RS
2239:RR
1958:.
1950:.
1942:.
1928:.
1904:.
1896:.
1888:.
1874:.
1851:.
1841:.
1833:.
1819:.
1815:.
1792:.
1784:.
1776:.
1762:.
1747:^
1733:.
1721:.
1698:.
1688:.
1676:.
1672:.
1654:^
1638:25
1636:.
1624:^
1606:.
1583:.
1573:81
1571:.
1559:^
1524:.
1499:.
1468:.
1460:.
1450:.
1440:87
1438:.
1434:.
1420:^
1402:.
1379:.
1371:.
1363:.
1349:.
1337:^
1319:.
1307:^
1293:.
1285:.
1277:.
1263:.
1249:^
1235:.
1227:.
1219:.
1205:.
1193:^
1179:.
1171:.
1163:.
1149:.
1126:.
1099:.
1095:.
1082:^
1064:.
1050:^
1034:44
1032:.
1009:.
1005:.
993:^
979:.
971:.
963:.
949:.
933:^
921:.
748:II
690:.
658:.
644:.
514:HR
498:GC
482:HD
478:BD
470:AG
456:,
327:ā5
309:pc
278:yr
262:yr
232:(R
2394:c
2374:e
2369:d
2364:c
2234:W
2229:V
2224:U
2219:T
2214:S
2209:R
2171:Ļ
2166:Ļ
2161:Ļ
2156:Ļ
2151:Ļ
2146:Īæ
2141:Ī¾
2136:Ī½
2131:Ī½
2126:Ī¼
2121:Ī»
2116:Īŗ
2111:Ī¹
2106:Īø
2101:Ī·
2096:Ī¶
2091:Ī¶
2086:Īµ
2081:Ī“
2076:Ī³
2010:e
2003:t
1996:v
1966:.
1954::
1946::
1936::
1912:.
1900::
1892::
1882::
1859:.
1845::
1837::
1827::
1800:.
1788::
1780::
1770::
1741:.
1737::
1729::
1706:.
1692::
1684::
1648:.
1644::
1618:.
1614::
1591:.
1587::
1579::
1536:.
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