61:
640:
705:
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.
790:
68:
1101:
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
704:
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
672:
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
1768:
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.;
662:. 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
772:
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
677:. 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
1934:
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".
592:, 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
658:
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
910:, 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
1102:
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).
1769:
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?".
887:
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
496:
536:
2579:
616:
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.
429:
769:. 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.
2019:
797:
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
2049:
823:
The distance of R Coronae
Borealis is not known exactly, but is estimated at 1.4 kiloparsecs from assumptions about its intrinsic brightness. The
2564:
2584:
697:, resulting in much of the star's light being blocked. The gradual restoration to normal brightness results from the dust being dispersed by
2574:
906:
from R Coronae Borealis, corresponding to a stream of fine dust (composed of grains about 5 nm in diameter) associated with the star's
2044:
1443:"On the Periodical Changes of Brightness of Two Fixed Stars. By Edward Pigott, Esq. Communicated by Sir Henry C. Englefield, Bart. F. R. S"
1270:
Montiel, Edward J.; Clayton, Geoffrey C.; Marcello, Dominic C.; Lockman, Felix J. (2015). "What is the Shell Around R Coronae Borealis?".
1012:
Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)".
1156:
White, Russel J.; Gabor, Jared M.; Hillenbrand, Lynne A. (2007). "High-Dispersion Optical Spectra of Nearby Stars Younger Than the Sun".
956:
Gaia Collaboration; et al. (November 2016). "Gaia Data Release 1. Summary of the astrometric, photometric, and survey properties".
1515:
480:
883:
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
1824:"Post-merger evolution of carbon-oxygen + helium white dwarf binaries and the origin of R Coronae Borealis and extreme helium stars"
876:
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
623:, "Variable (star) of Corona (Borealis)". It has also been called a "reverse nova" because of its habit of fading from sight. The
2039:
2604:
2594:
89:
1881:
StasiÅska, G.; Szczerba, R.; Schmidt, M.; SiĆ³dmiak, N. (2006). "Post-AGB stars as testbeds of nucleosynthesis in AGB stars".
1409:
Asplund, M.; Gustafsson, B.; Lambert, D. L.; Rao, N. K. (2000). "The R Coronae Borealis stars - atmospheres and abundances".
1356:
Clayton, Geoffrey C.; Geballe, T. R.; Zhang, Wanshu (2013). "Variable Winds and Dust Formation in R Coronae Borealis Stars".
588:
at irregular intervals. R Coronae Borealis itself normally shines at approximately magnitude 6, just about visible to the
2012:
628:
2589:
577:
221:
31:
2599:
2364:
2354:
831:
whose distances are known quite accurately. The luminosity is estimated from helium star models to be 19,000
1071:
Ducati, J. R. (2002). "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system".
2211:
624:
468:
2569:
2359:
2181:
2156:
2096:
2005:
1613:
Skuljan, L.; Cottrell, P. L. (2002). "Recent declines of RS Telescopii, UW Centauri, and V Coronae Australis".
921:
from the surface, and are visible as cometary knots when they lie to side of the star. There is also a 2
852:
There is a fainter star 3" away from R Coronae Borealis, but it is believed to be a distant class K dwarf. Its
619:
At its discovery it was described simply as "the variable in the Northern crown". It was later referred to as
1133:
Mattei, Janet A.; Waagen, Elizabeth O.; Foster, E. Grant (1991). "R Coronae Borealis light curves 1843-1990".
765:, and other metals. The lines are typically very narrow at this stage. Helium emission lines sometimes show
2131:
2609:
2384:
2379:
2374:
2369:
2274:
2171:
2126:
2116:
2091:
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2076:
902:
Direct imaging with the Hubble Space Telescope shows extensive dust clouds out to a radius of around 2000
828:
508:
492:
151:
2431:
2191:
2121:
2106:
2101:
2081:
524:
472:
437:
849:
data release 1 parallax also gives a distance of 1.4 kpc although with a considerable margin of error.
557:
651:
in 1795. In 1935 it was the first star shown to have a different chemical composition to the Sun via
60:
2176:
2166:
2146:
2141:
2111:
1954:
1900:
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1289:
1231:
1175:
1138:
1115:
1080:
1048:
1021:
975:
312:
42:
745:
are also present. The spectrum is variable, most obviously during the brightness fades. The normal
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2259:
2254:
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2161:
2151:
2136:
798:
746:
512:
38:
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327:
134:
1645:
The Society for Astronomical Sciences 25th Annual Symposium on Telescope Science. Held May 23ā25
914:
regions in an expanding front. "Puffs" of dust emitted from the star condense at about 85
2346:
2068:
1511:
1507:
1500:
903:
846:
816:
at maximum is reasonably well known at 6,900K and appears to decrease during the fades as the
609:
85:
2539:
1962:
1958:
1908:
1904:
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1796:
1745:
1700:
1595:
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1235:
1183:
983:
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929:
714:
404:
296:
1103:
643:
Light curve of R Coronae Borealis from 1990 to 2017, showing the unprecedented deep minimum
596:", after the more common type of star which rapidly increases in brightness before fading.
2475:
2028:
1578:
Berman, Louis (1935). "The Spectrum Analysis of the Hot Carbon Star, R Coronae Borealis".
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1339:
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1179:
1142:
1119:
1084:
1052:
1025:
2499:
613:
604:
R Coronae Borealis is a faint naked eye star, but does not have any traditional names.
488:
455:
304:
284:
268:
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1867:
1808:
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1714:
1484:
1395:
1387:
1309:
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659:
648:
581:
257:
216:
97:
1974:
1920:
1251:
1997:
995:
907:
873:
778:
686:
652:
605:
384:
357:
1966:
1195:
1104:"VizieR Online Data Catalog: 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)"
987:
789:
1912:
1559:
1243:
1014:
VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S
2200:
911:
869:
853:
817:
813:
774:
206:
195:
184:
173:
162:
123:
2534:
2529:
2524:
2519:
2514:
2308:
868:
There are two main models for the formation of R CrB stars: the merger of two
674:
569:
397:
364:
228:
2400:
2337:
2287:
2282:
1858:
1823:
589:
1467:
1326:
Saio, H. (2008). "Radial and Nonradial Pulsations in RCB and EHe-B Stars".
647:
The variability of R Coronae Borealis was discovered by English astronomer
860:
are not consistent with being at the same distance as R Coronae Borealis.
2459:
2454:
2449:
2444:
2439:
2318:
2303:
1895:
726:
718:
2485:
2480:
2313:
1728:
Searle, Leonard (1961). "An Abundance Analysis of R Coronae Borealis".
884:
742:
1476:
717:
a late F or early G yellow supergiant, but with marked peculiarities.
2422:
1643:
Watson, C. L. (2006). "The International Variable Star Index (VSX)".
1212:
Van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction".
928:
shell about 4 pc wide containing dust at 25 K, which may be a fossil
734:
722:
690:
678:
551:
444:
377:
319:
17:
1442:
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970:
2408:
1991:
1949:
1840:
1783:
1681:"Optical Spectroscopy at Deep Light Minimum of R Coronae Borealis"
1370:
1226:
1170:
788:
738:
638:
528:
516:
476:
67:
2323:
2059:
694:
593:
532:
520:
288:
272:
2001:
1039:
Klochkova, V. G. (1997). "Supergiants with large IR excesses".
827:
of ā5 is calculated by comparison with R CrB variables in the
1679:
Howell, Steve B.; Rector, Travis A.; Walter, Donald (2013).
685:. The sudden drop in brightness may be caused by a rapid
1447:
Philosophical Transactions of the Royal Society of London
1685:
Publications of the Astronomical Society of the Pacific
30:
This article is about the star. For the star type, see
1822:
Zhang, X.; Jeffery, C. S.; Chen, X.; Han, Z. (2014).
627:
R Coronae Borealis was introduced, as "Coronae R" by
894:
for R CrB, but with a considerable margin of error.
2507:
2498:
2468:
2430:
2421:
2393:
2345:
2336:
2296:
2273:
2210:
2190:
2067:
2058:
1531:Bone, Neil (2006). "Skky notes for April and May".
1499:
27:Variable star in the constellation Corona Borealis
1828:Monthly Notices of the Royal Astronomical Society
1041:Bulletin of the Special Astrophysical Observatory
1533:Journal of the British Astronomical Association
1351:
1349:
1328:Hydrogen-Deficient Stars ASP Conference Series
805:suggests that the star's mass is 0.8-0.9
713:R Coronae Borealis at maximum light shows the
612:designation although it is marked on his map.
2013:
1441:Pigott, Edward; Englefield, Henry C. (1797).
8:
128:+28° 09′ 24.295″
1207:
1205:
1108:CDS/ADC Collection of Electronic Catalogues
1073:CDS/ADC Collection of Electronic Catalogues
88:J2000.0
2504:
2427:
2342:
2064:
2020:
2006:
1998:
1763:
1761:
1759:
838:and the star has a radius around 100
1948:
1894:
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1839:
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1704:
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1670:
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1369:
1283:
1265:
1263:
1261:
1225:
1169:
969:
1066:
1064:
1062:
77:Location of R Coronae Borealis (circled)
2580:Objects with variable star designations
1561:Humboldts Kosmos: In verkĆ¼rzter Gestalt
1321:
1319:
1096:
1094:
941:
264:
1638:
1636:
1007:
1005:
47:
951:
949:
947:
945:
7:
2045:Corona Borealis in Chinese astronomy
2050:HerculesāCorona Borealis Great Wall
1506:. Dover Publications, Inc. p.
793:R Coronae Borealis in optical light
276:
1502:Star Names: Their Lore and Meaning
25:
1992:AAVSO Variable Star of the Season
503: 2039-1605-1, CDS 886,
2040:List of stars in Corona Borealis
2029:Constellation of Corona Borealis
820:is obscured by condensing dust.
721:lines are weak or absent, while
66:
59:
1558:Alexander von Humboldt (1850).
2565:Henry Draper Catalogue objects
1453:. The Royal Society: 133ā141.
576:. It is the prototype of the
1:
2585:Bright Star Catalogue objects
725:lines and molecular bands of
572:star in the constellation of
2575:R Coronae Borealis variables
1937:Astronomy & Astrophysics
958:Astronomy & Astrophysics
629:Friedrich Wilhelm Argelander
1967:10.1051/0004-6361/201117138
988:10.1051/0004-6361/201629512
733:are exceptionally strong.
578:R Coronae Borealis variable
303:0.73 Ā± 0.27
32:R Coronae Borealis variable
2626:
1913:10.1051/0004-6361:20053553
1883:Astronomy and Astrophysics
1801:10.1088/0004-637X/743/1/44
1411:Astronomy and Astrophysics
1388:10.1088/0004-6256/146/2/23
1302:10.1088/0004-6256/150/1/14
1244:10.1051/0004-6361:20078357
1214:Astronomy and Astrophysics
36:
29:
2035:
1771:The Astrophysical Journal
1580:The Astrophysical Journal
625:variable star designation
544:
479: J15483440+2809242,
461:
454:
450:
351:
346:
342:
234:
227:
145:
82:
53:
1358:The Astronomical Journal
1272:The Astronomical Journal
1158:The Astronomical Journal
781:lines visible at times.
584:, which fade by several
37:Not to be confused with
1959:2012A&A...539A..56J
1905:2006A&A...450..701S
1564:. Greiner und Pfeiffer.
1423:2000A&A...353..287A
1236:2007A&A...474..653V
980:2016A&A...595A...2G
328:Absolute magnitude
135:Apparent magnitude
2605:IRAS catalogue objects
2595:Durchmusterung objects
1468:10.1098/rstl.1797.0007
898:Circumstellar material
829:Large Magellanic Cloud
794:
693:-rich dust similar to
644:
1859:10.1093/mnras/stu1741
1730:Astrophysical Journal
1498:Allen, R. H. (1963).
792:
642:
568:is a low-mass yellow
2370:Ļ Coronae Borealis b
2365:Īæ Coronae Borealis b
2360:Īŗ Coronae Borealis b
2355:Īµ Coronae Borealis b
43:Rho Coronae Borealis
1850:2014MNRAS.445..660Z
1793:2011ApJ...743...44C
1742:1961ApJ...133..531S
1697:2013PASP..125..879H
1657:2006SASS...25...47W
1627:2002Obs...122..322S
1592:1935ApJ....81..369B
1545:2006JBAA..116..102B
1459:1797RSPT...87..133P
1380:2013AJ....146...23C
1340:2008ASPC..391...69S
1294:2015AJ....150...14M
1180:2007AJ....133.2524W
1143:1991rcbl.book.....M
1120:2003yCat.2246....0C
1085:2002yCat.2237....0D
1053:1997BSAO...44....5K
1026:2009yCat....102025S
799:extreme helium star
747:absorption spectrum
681:dust in the star's
545:Database references
487: 02039-01605,
475: N1330022410,
50:
49:R Coronae Borealis
39:RR Coronae Borealis
2590:G-type supergiants
904:astronomical units
858:apparent magnitude
825:absolute magnitude
795:
699:radiation pressure
645:
621:Variabilis Coronae
608:did not give it a
566:R Coronae Borealis
535: 15465+2818,
456:Other designations
217:Variable type
152:Spectral type
48:
2600:Hipparcos objects
2552:
2551:
2548:
2547:
2494:
2493:
2417:
2416:
2332:
2331:
2324:XO-1 (Moldoveanu)
872:; or a very late
653:spectral analysis
563:
562:
267: -2.10
16:(Redirected from
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2505:
2428:
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2015:
2008:
1999:
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1978:
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1896:astro-ph/0601504
1878:
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1691:(930): 879ā888.
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1199:
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1164:(6): 2524ā2536.
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1123:
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1089:
1088:
1068:
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1000:
999:
973:
953:
930:planetary nebula
801:. Modelling the
767:P Cygni profiles
531: 1544+28A,
491:+28Ā° 2477,
483:+28Ā° 1513,
465:Coronae Borealis
282:
278:
266:
146:Characteristics
138:
118:
113:
83:Observation data
70:
63:
51:
21:
2625:
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2619:
2618:
2616:
2615:
2614:
2570:Corona Borealis
2555:
2554:
2553:
2544:
2540:RX J1532.9+3021
2500:Galaxy clusters
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2413:
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1615:The Observatory
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1135:AAVSO Monograph
1132:
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1092:
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866:
844:
841:
837:
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808:
787:
764:
760:
756:
753:, especially He
749:is replaced by
732:
711:
668:
665:
637:
602:
574:Corona Borealis
540:
418:Surface gravity
410:
407:
390:
387:
370:
367:
333:
280:
275:
251:27.83 km/s
246:
241:Radial velocity
133:
116:
111:Right ascension
109:
103:Corona Borealis
84:
78:
76:
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73:
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35:
28:
23:
22:
15:
12:
11:
5:
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2546:
2545:
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2527:
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2511:
2509:
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2496:
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2483:
2478:
2476:FSC 15307+3253
2472:
2470:
2466:
2465:
2463:
2462:
2457:
2452:
2447:
2442:
2436:
2434:
2425:
2419:
2418:
2415:
2414:
2412:
2411:
2409:XO-1b (Negoiu)
2406:
2403:
2397:
2395:
2391:
2390:
2388:
2387:
2382:
2377:
2372:
2367:
2362:
2357:
2351:
2349:
2340:
2334:
2333:
2330:
2329:
2327:
2326:
2321:
2316:
2311:
2306:
2300:
2298:
2294:
2293:
2291:
2290:
2288:145457 (Kamuy)
2285:
2279:
2277:
2271:
2270:
2268:
2267:
2262:
2257:
2252:
2247:
2242:
2237:
2232:
2227:
2222:
2216:
2214:
2208:
2207:
2205:
2204:
2196:
2194:
2188:
2187:
2185:
2184:
2179:
2174:
2169:
2164:
2159:
2154:
2149:
2144:
2139:
2134:
2129:
2124:
2119:
2114:
2109:
2104:
2099:
2094:
2089:
2084:
2079:
2073:
2071:
2062:
2056:
2055:
2053:
2052:
2047:
2042:
2036:
2033:
2032:
2027:
2025:
2024:
2017:
2010:
2002:
1996:
1995:
1994:, January 2000
1987:
1986:External links
1984:
1981:
1980:
1926:
1873:
1834:(1): 660ā673.
1814:
1755:
1750:10.1086/147056
1720:
1706:10.1086/672163
1662:
1632:
1605:
1600:10.1086/143644
1567:
1550:
1523:
1517:978-0486210797
1516:
1490:
1428:
1401:
1345:
1315:
1257:
1220:(2): 653ā664.
1201:
1188:10.1086/514336
1148:
1125:
1090:
1058:
1031:
1001:
940:
939:
937:
934:
925:
922:
918:
915:
899:
896:
891:
888:
880:
877:
865:
862:
842:
839:
835:
832:
809:
806:
786:
783:
762:
758:
754:
751:emission lines
730:
710:
707:
666:
663:
636:
633:
614:John Flamsteed
601:
598:
582:variable stars
561:
560:
555:
547:
546:
542:
541:
507: 104338,
495: 141527,
462:
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55:
54:
26:
24:
14:
13:
10:
9:
6:
4:
3:
2:
2622:
2611:
2610:2MASS objects
2608:
2606:
2603:
2601:
2598:
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2593:
2591:
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2586:
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2256:
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2238:
2236:
2233:
2231:
2228:
2226:
2223:
2221:
2218:
2217:
2215:
2213:
2209:
2203:
2202:
2198:
2197:
2195:
2193:
2189:
2183:
2180:
2178:
2175:
2173:
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2165:
2163:
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2138:
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2128:
2125:
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2110:
2108:
2105:
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2100:
2098:
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1993:
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1968:
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1023:
1019:
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1008:
1006:
1002:
997:
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989:
985:
981:
977:
972:
967:
963:
959:
952:
950:
948:
946:
942:
935:
933:
931:
913:
909:
905:
897:
895:
886:
875:
871:
863:
861:
859:
855:
850:
848:
830:
826:
821:
819:
815:
804:
800:
791:
784:
782:
780:
779:chromospheric
776:
770:
768:
752:
748:
744:
740:
736:
728:
724:
720:
716:
708:
706:
702:
700:
696:
692:
688:
684:
680:
676:
670:
661:
660:RY Sagittarii
656:
654:
650:
649:Edward Pigott
641:
634:
632:
630:
626:
622:
617:
615:
611:
607:
599:
597:
595:
591:
587:
583:
579:
575:
571:
567:
559:
556:
554:
553:
549:
548:
543:
539: 84015.
538:
534:
530:
526:
522:
518:
515: 77442,
514:
511: 21257,
510:
506:
502:
499: 3581,
498:
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490:
486:
482:
478:
474:
470:
466:
460:
457:
453:
449:
446:
442:
440:
439:
435:
434:
431:
427:
425:
423:
419:
415:
414:
411:
403:~10,000
402:
400:
399:
395:
394:
391:
382:
380:
379:
375:
374:
371:
363:0.8-0.9
362:
360:
359:
355:
354:
350:
345:
341:
337:
335:
329:
325:
324:
321:
317:
315:
314:
310:
309:
306:
302:
300:
298:
294:
293:
290:
286:
274:
270:
263:
261:
259:
258:Proper motion
255:
254:
250:
248:
242:
238:
237:
233:
230:
226:
223:
220:
218:
215:
214:
210:
208:
204:
203:
199:
197:
193:
192:
188:
186:
182:
181:
177:
175:
171:
170:
166:
164:
160:
159:
155:
153:
150:
149:
144:
140:
136:
132:
131:
127:
125:
122:
121:
117:15 48 34.4147
115:
112:
108:
107:
104:
101:
99:
98:Constellation
96:
95:
91:
87:
81:
69:
62:
52:
44:
40:
33:
19:
2219:
2199:
2077:Ī± (Alphecca)
1943:(A56): A56.
1940:
1936:
1929:
1886:
1882:
1876:
1831:
1827:
1817:
1774:
1770:
1733:
1729:
1723:
1688:
1684:
1648:
1644:
1618:
1614:
1608:
1583:
1579:
1560:
1553:
1536:
1532:
1526:
1501:
1493:
1450:
1446:
1414:
1410:
1404:
1361:
1357:
1331:
1327:
1275:
1271:
1217:
1213:
1161:
1157:
1151:
1134:
1128:
1111:
1107:
1076:
1072:
1044:
1040:
1034:
1017:
1013:
961:
957:
908:stellar wind
901:
874:helium flash
870:white dwarfs
867:
851:
822:
796:
771:
712:
703:
687:condensation
671:
657:
646:
620:
618:
610:Greek letter
606:Johann Bayer
603:
600:Nomenclature
565:
564:
550:
527: 5880,
523: 9116,
519: 4219,
436:
421:
416:
396:
376:
356:
326:
311:
295:
256:
239:
141:5.71 - 14.8
2082:Ī² (Nusakan)
818:photosphere
814:temperature
775:photosphere
675:wavelengths
635:Variability
471: CrB,
443:6,750
438:Temperature
318:1,400
207:color index
196:color index
185:color index
174:color index
163:color index
124:Declination
2559:Categories
2338:Exoplanets
2309:Gliese 611
1889:(2): 701.
1539:(2): 102.
1285:1505.04173
1114:: II/246.
971:1609.04172
936:References
803:pulsations
785:Properties
777:, leaving
737:lines and
729:(CN) and C
683:atmosphere
586:magnitudes
570:supergiant
420:(log
398:Luminosity
229:Astrometry
2401:GJ 3929 b
2192:Flamsteed
1950:1203.1265
1868:118506564
1841:1408.5500
1809:119240518
1784:1110.3235
1777:(1): 44.
1715:120129277
1485:186214528
1396:118385818
1371:1305.5047
1364:(2): 23.
1310:119271048
1278:(1): 14.
1227:0708.1752
1171:0706.0542
864:Formation
631:in 1850.
590:naked eye
428:0.5
137: (V)
2423:Galaxies
2319:NGC 6002
2304:ADS 9731
2212:Variable
1975:55589182
1921:12040452
1252:18759600
926:☉
919:☉
892:☉
881:☉
843:☉
836:☉
810:☉
741:such as
727:cyanogen
719:Hydrogen
715:spectrum
709:Spectrum
667:☉
409:☉
389:☉
383:85
369:☉
330: (M
313:Distance
297:Parallax
92:J2000.0
2486:IC 4539
2481:IC 1166
2314:GJ 3929
1955:Bibcode
1901:Bibcode
1846:Bibcode
1789:Bibcode
1738:Bibcode
1736:: 531.
1693:Bibcode
1653:Bibcode
1623:Bibcode
1621:: 322.
1588:Bibcode
1586:: 369.
1541:Bibcode
1455:Bibcode
1419:Bibcode
1417:: 287.
1376:Bibcode
1336:Bibcode
1290:Bibcode
1232:Bibcode
1176:Bibcode
1139:Bibcode
1116:Bibcode
1081:Bibcode
1049:Bibcode
1022:Bibcode
996:1828208
976:Bibcode
885:lithium
845:. The
812:. The
743:calcium
673:longer
463:R
347:Details
90:Equinox
2283:140913
2201:23 Her
1973:
1919:
1866:
1807:
1713:
1651:: 47.
1514:
1483:
1477:106921
1475:
1394:
1334:: 69.
1308:
1250:
1196:122854
1194:
994:
964:: 23.
854:colour
739:metals
735:Helium
723:carbon
691:carbon
679:carbon
552:SIMBAD
378:Radius
283:
281:ā11.52
279:
211:0.800
200:0.275
156:G0Iep
2508:Abell
2469:Other
2394:Other
2347:Bayer
2297:Other
2069:Bayer
2060:Stars
1971:S2CID
1945:arXiv
1917:S2CID
1891:arXiv
1864:S2CID
1836:arXiv
1805:S2CID
1779:arXiv
1711:S2CID
1481:S2CID
1473:JSTOR
1392:S2CID
1366:arXiv
1306:S2CID
1280:arXiv
1248:S2CID
1222:arXiv
1192:S2CID
1166:arXiv
1079:: 0.
1047:: 5.
998:. A2.
992:S2CID
966:arXiv
912:shock
529:AAVSO
517:RAFGL
477:2MASS
277:Dec.:
222:R CrB
189:0.45
178:0.60
167:0.13
86:Epoch
18:R CrB
2535:2162
2530:2142
2525:2067
2520:2065
2515:2061
2460:6122
2455:6120
2450:6104
2445:6086
2440:6085
1512:ISBN
1112:2246
1077:2237
856:and
847:Gaia
761:, Na
757:, Ca
695:soot
594:nova
558:data
533:IRAS
521:GCRV
473:GSC2
358:Mass
205:JāK
194:JāH
183:VāR
172:BāV
161:UāB
2432:NGC
1963:doi
1941:539
1909:doi
1887:450
1854:doi
1832:445
1797:doi
1775:743
1746:doi
1734:133
1701:doi
1689:125
1619:122
1596:doi
1537:116
1508:178
1463:doi
1415:353
1384:doi
1362:146
1332:391
1298:doi
1276:150
1240:doi
1218:474
1184:doi
1162:133
984:doi
962:595
689:of
580:of
537:SAO
513:HIP
505:PPM
501:TYC
497:PLX
485:GSC
430:cgs
305:mas
299:(Ļ)
285:mas
269:mas
265:RA:
260:(Ī¼)
41:or
2561::
2275:HD
2265:UW
2260:TY
2255:RS
2250:RR
1969:.
1961:.
1953:.
1939:.
1915:.
1907:.
1899:.
1885:.
1862:.
1852:.
1844:.
1830:.
1826:.
1803:.
1795:.
1787:.
1773:.
1758:^
1744:.
1732:.
1709:.
1699:.
1687:.
1683:.
1665:^
1649:25
1647:.
1635:^
1617:.
1594:.
1584:81
1582:.
1570:^
1535:.
1510:.
1479:.
1471:.
1461:.
1451:87
1449:.
1445:.
1431:^
1413:.
1390:.
1382:.
1374:.
1360:.
1348:^
1330:.
1318:^
1304:.
1296:.
1288:.
1274:.
1260:^
1246:.
1238:.
1230:.
1216:.
1204:^
1190:.
1182:.
1174:.
1160:.
1137:.
1110:.
1106:.
1093:^
1075:.
1061:^
1045:44
1043:.
1020:.
1016:.
1004:^
990:.
982:.
974:.
960:.
944:^
932:.
759:II
701:.
669:.
655:.
525:HR
509:GC
493:HD
489:BD
481:AG
467:,
338:ā5
320:pc
289:yr
273:yr
243:(R
2405:c
2385:e
2380:d
2375:c
2245:W
2240:V
2235:U
2230:T
2225:S
2220:R
2182:Ļ
2177:Ļ
2172:Ļ
2167:Ļ
2162:Ļ
2157:Īæ
2152:Ī¾
2147:Ī½
2142:Ī½
2137:Ī¼
2132:Ī»
2127:Īŗ
2122:Ī¹
2117:Īø
2112:Ī·
2107:Ī¶
2102:Ī¶
2097:Īµ
2092:Ī“
2087:Ī³
2021:e
2014:t
2007:v
1977:.
1965::
1957::
1947::
1923:.
1911::
1903::
1893::
1870:.
1856::
1848::
1838::
1811:.
1799::
1791::
1781::
1752:.
1748::
1740::
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