317:
497:
than many supergiants. Classification is complex and difficult with small differences between luminosity classes and a continuous range of intermediate forms. The most massive stars develop giant or supergiant spectral features while still burning hydrogen in their cores, due to mixing of heavy elements to the surface and high luminosity which produces a powerful stellar wind and causes the star's atmosphere to expand.
2877:
32:
2927:
447:, but most of the energy goes into lifting the degeneracy and the core becomes convective. The energy generated by helium fusion reduces the pressure in the surrounding hydrogen-burning shell, which reduces its energy-generation rate. The overall luminosity of the star decreases, its outer envelope contracts again, and the star moves from the red-giant branch to the
2951:
2915:
2939:
2888:
466:(AGB) analogous to the red-giant branch but more luminous, with a hydrogen-burning shell contributing most of the energy. Stars only remain on the AGB for around a million years, becoming increasingly unstable until they exhaust their fuel, go through a planetary nebula phase, and then become a carbonâoxygen white dwarf.
496:
O class main sequence stars are already highly luminous. The giant phase for such stars is a brief phase of slightly increased size and luminosity before developing a supergiant spectral luminosity class. Type O giants may be more than a hundred thousand times as luminous as the sun, brighter
481:
are already very luminous and they move horizontally across the HR diagram when they leave the main sequence, briefly becoming blue giants before they expand further into blue supergiants. They start core-helium burning before the core becomes degenerate and develop smoothly into red supergiants
735:
Giant stars with intermediate temperatures (spectral class G, F, and at least some A) are called yellow giants. They are far less numerous than red giants, partly because they only form from stars with somewhat higher masses, and partly because they spend less time in that phase of their lives.
492:
range have somewhat intermediate properties and have been called super-AGB stars. They largely follow the tracks of lighter stars through RGB, HB, and AGB phases, but are massive enough to initiate core carbon burning and even some neon burning. They form oxygenâmagnesiumâneon cores, which may
770:
Yellow giants may be moderate-mass stars evolving for the first time towards the red-giant branch, or they may be more evolved stars on the horizontal branch. Evolution towards the red-giant branch for the first time is very rapid, whereas stars can spend much longer on the horizontal branch.
819:. Higher-mass stars leave the main sequence to become blue giants, then bright blue giants, and then blue supergiants, before expanding into red supergiants, although at the very highest masses the giant stage is so brief and narrow that it can hardly be distinguished from a blue supergiant.
686:. The RGB stars are by far the most common type of giant star due to their moderate mass, relatively long stable lives, and luminosity. They are the most obvious grouping of stars after the main sequence on most HR diagrams, although white dwarfs are more numerous but far less luminous.
560:
Subgiants are an entirely separate spectroscopic luminosity class (IV) from giants, but share many features with them. Although some subgiants are simply over-luminous main-sequence stars due to chemical variation or age, others are a distinct evolutionary track towards true giants.
461:
has a carbonâoxygen core that becomes degenerate and starts helium burning in a shell. As with the earlier collapse of the helium core, this starts convection in the outer layers, triggers a second dredge-up, and causes a dramatic increase in size and luminosity. This is the
524:. They steadily become hotter and more luminous throughout this time. Eventually they do develop a radiative core, subsequently exhausting hydrogen in the core and burning hydrogen in a shell surrounding the core. (Stars with a mass in excess of 0.16
482:
without a strong increase in luminosity. At this stage they have comparable luminosities to bright AGB stars although they have much higher masses, but will further increase in luminosity as they burn heavier elements and eventually become a supernova.
402:
where it will stably burn hydrogen in a shell for a substantial fraction of its entire life (roughly 10% for a Sun-like star). The core continues to gain mass, contract, and increase in temperature, whereas there is some mass loss in the outer layers.
740:
on the HR diagram where the majority of stars are pulsating variables. The instability strip reaches from the main sequence up to hypergiant luminosities, but at the luminosities of giants there are several classes of pulsating variable stars:
665:
Within any giant luminosity class, the cooler stars of spectral class K, M, S, and C, (and sometimes some G-type stars) are called red giants. Red giants include stars in a number of distinct evolutionary phases of their lives: a main
394:, rapidly collapses, and may become degenerate. This causes the outer layers to expand even further and generates a strong convective zone that brings heavy elements to the surface in a process called the first
390:
it does not become hot enough to start helium burning (higher-mass stars are supergiants and evolve differently). Instead, after just a few million years the core reaches the
531:
may expand at this point, but will never become very large.) Shortly thereafter, the star's supply of hydrogen will be completely exhausted and it is expected to become a
308:
A hot, luminous main-sequence star may also be referred to as a giant, but any main-sequence star is properly called a dwarf, regardless of how large and luminous it is.
2728:
682:(AGB), although AGB stars are often large enough and luminous enough to get classified as supergiants; and sometimes other large cool stars such as immediate
375:
in a shell around the core. The portion of the star outside the shell expands and cools, but with only a small increase in luminosity, and the star becomes a
398:. This strong convection also increases the transport of energy to the surface, the luminosity increases dramatically, and the star moves onto the
2760:
815:
The blue giants are a very heterogeneous grouping, ranging from high-mass, high-luminosity stars just leaving the main sequence to low-mass,
391:
736:
However, they include a number of important classes of variable stars. High-luminosity yellow stars are generally unstable, leading to the
2735:
2054:
1294:
1073:
1039:
1003:
931:
903:
421:. According to stellar evolution theory, no star of such low mass can have evolved to that stage within the age of the Universe.
2447:
1134:
259:
36:
2361:
417:. It will therefore remain a hydrogen-fusing red giant until it runs out of hydrogen, at which point it will become a helium
2740:
2377:
1396:
748:, pulsating horizontal-branch class A (sometimes F) stars with periods less than a day and amplitudes of a magnitude of less;
604:
383:
core continues to grow and increase in temperature as it accretes helium from the shell, but in stars up to about 10-12
546:
There are a wide range of giant-class stars and several subdivisions are commonly used to identify smaller groups of stars.
2787:
2654:
995:
538:, although the universe is too young for any such star to exist yet, so no star with that history has ever been observed.
322:
316:
2905:
1162:
Eldridge, J.J.; Tout, C.A. (2004). "Exploring the divisions and overlap between AGB and super-AGB stars and supernovae".
2770:
2721:
2696:
1989:
2074:
2711:
2691:
874:
512:
will not become a giant star at all. For most of their lifetimes, such stars have their interior thoroughly mixed by
822:
Lower-mass, core-helium-burning stars evolve from red giants along the horizontal branch and then back again to the
2775:
2706:
2676:
757:
2782:
2659:
2636:
2218:
1667:
1662:
1657:
1652:
1647:
1642:
1313:
Mazumdar, A.; et al. (August 2009), "Asteroseismology and interferometry of the red giant star É Ophiuchi",
1205:
1925:
1799:
1434:
1089:
2452:
2121:
2701:
2251:
2161:
2103:
2029:
1600:
1526:
823:
679:
463:
255:
1476:
2862:
2842:
2614:
2609:
2402:
2351:
2156:
2146:
1819:
1617:
1585:
1459:
43:
611:, based on the appearance of their spectra. The bright giant luminosity class was first defined in 1943.
2716:
2686:
2681:
2671:
2599:
2387:
1553:
1368:
1141:
628:
247:
1834:
947:
Russell, Henry Norris (1914). "Relations
Between the Spectra and Other Characteristics of the Stars".
2976:
2857:
2755:
2745:
2594:
2562:
2356:
2151:
2136:
1449:
1332:
1255:
1214:
1181:
1105:
991:
956:
763:
440:
1696:
2971:
2955:
2457:
2317:
2300:
1971:
1873:
751:
648:
2943:
2931:
2852:
2813:
2765:
2750:
2664:
2604:
2527:
2437:
2407:
2397:
2341:
2263:
1954:
1590:
1389:
1348:
1322:
1171:
206:
493:
collapse in an electron-capture supernova, or they may leave behind an oxygenâneon white dwarf.
754:, more-luminous pulsating variables also known as type II Cepheids, with periods of 10â20 days;
2803:
2288:
2228:
2201:
2181:
1981:
1765:
1753:
1580:
1560:
1514:
1496:
1464:
1290:
1069:
1035:
1027:
1009:
999:
927:
899:
816:
745:
737:
671:
448:
283:
2919:
2631:
2584:
2534:
2522:
2500:
2495:
2422:
2382:
2329:
2111:
2034:
2009:
1903:
1824:
1548:
1509:
1340:
1336:
1263:
1222:
1113:
699:
2818:
2621:
2490:
2334:
2305:
2246:
2241:
2116:
1844:
1809:
1743:
1689:
1684:
1629:
1439:
568:
185:
1259:
1218:
1185:
1109:
960:
2880:
2646:
2485:
2312:
2283:
2258:
2191:
1880:
1748:
1634:
1536:
1426:
1416:
851:
784:
778:
643:
372:
335:
192:
2965:
2832:
2626:
2589:
2557:
2432:
2141:
1964:
1935:
1913:
1531:
1504:
1481:
1382:
979:
835:
771:
Horizontal-branch stars, with more heavy elements and lower mass, are more unstable.
693:
683:
638:
633:
580:
339:
279:
237:
141:
1352:
1145:
1093:
2892:
2567:
2517:
2512:
2412:
2295:
2278:
2236:
2196:
2131:
2014:
1959:
1940:
1920:
1898:
1890:
1733:
1726:
1565:
1486:
1469:
975:
444:
355:
278:
were coined for stars of quite different luminosity despite similar temperature or
178:
106:
99:
92:
85:
78:
71:
64:
57:
50:
1344:
1284:
2808:
2507:
2480:
2472:
2462:
2442:
2417:
2346:
2268:
2024:
1999:
1994:
1908:
1868:
1829:
1794:
1777:
1772:
1444:
827:
808:
The hottest giants, of spectral classes O, B, and sometimes early A, are called
535:
418:
406:
If the star's mass, when on the main sequence, was below approximately 0.4
290:
120:
113:
31:
2392:
2089:
2062:
2039:
2019:
2004:
1856:
1760:
1738:
1716:
1575:
809:
803:
790:
608:
574:
513:
431:
the core temperature eventually reaches 10 K and helium will begin to fuse to
359:
302:
298:
242:
233:
199:
171:
2579:
2427:
2211:
2176:
2171:
2166:
2126:
2079:
2069:
1863:
1839:
1814:
1721:
1672:
1605:
1595:
1570:
1543:
1519:
1454:
1118:
1013:
723:
711:
675:
667:
660:
399:
395:
164:
127:
607:. These are stars which straddle the boundary between ordinary giants and
17:
2572:
2273:
1947:
1706:
1679:
1176:
855:
831:
812:. Sometimes A- and late-B-type stars may be referred to as white giants.
705:
555:
521:
376:
368:
331:
150:
134:
1286:
Classifying the Cosmos: How We Can Make Sense of the
Celestial Landscape
2847:
2322:
2084:
1851:
1804:
1787:
1782:
1701:
987:
760:, more luminous still and mostly supergiants, with even longer periods;
623:
618:
1199:
Laughlin, Gregory; Bodenheimer, Peter; Adams, Fred C. (10 June 1997).
2837:
2825:
2044:
1930:
861:
845:
532:
436:
432:
414:
380:
229:
2887:
1268:
1243:
1227:
1200:
1327:
454:
When the core helium is exhausted, a star with up to about 8
315:
516:
and so they can continue fusing hydrogen for a time in excess of
413:, it will never reach the central temperatures necessary to fuse
293:
and luminosities between 10 and a few thousand times that of the
2206:
2186:
1405:
717:
614:
Well known stars which are classified as bright giants include:
596:
343:
225:
1378:
505:
A star whose initial mass is less than approximately 0.25
2552:
294:
1244:"Line Broadening in High-Luminosity Stars. I. Bright Giants"
338:
at its core has been depleted and, as a result, leaves the
297:. Stars still more luminous than giants are referred to as
781:(Ï Octantis), an F-type giant and a Delta Scuti variable;
1374:
320:
Internal structure of a Sun-like star and a red giant.
720:(Îż Ceti), an M-type giant and prototype Mira variable.
2903:
854:(η Tauri), a B-type giant, the brightest star in the
830:
they can become blue giants. It is thought that some
371:
it contracts and heats up so that hydrogen starts to
289:
Giant stars have radii up to a few hundred times the
250:. They lie above the main sequence (luminosity class
474:
Main-sequence stars with masses above about 12
2796:
2645:
2543:
2471:
2370:
2227:
2102:
1980:
1889:
1616:
1495:
1425:
1308:
1306:
520:years, much longer than the current age of the
1068:. Chichester, UK: John Wiley & Sons, Ltd.
926:(5th ed.). New York: Facts On File, Inc.
27:Type of star, larger and brighter than the Sun
1390:
922:John Daintith and William Gould, ed. (2006).
443:. When the core is degenerate helium fusion
8:
766:, includes subgiant and main-sequence stars.
1064:Maurizio Salaris and Santi Cassisi (2005).
1622:
1397:
1383:
1375:
1164:Memorie della SocietĂ Astronomica Italiana
1066:Evolution of Stars and Stellar Populations
1326:
1267:
1226:
1175:
1117:
1094:"Structure and Evolution of White Dwarfs"
1034:. Cambridge: Cambridge University Press.
894:Patrick Moore, ed. (2002). "Giant star".
354:For a star with a mass above about 0.25
2910:
886:
1059:
1057:
1055:
1053:
1051:
917:
915:
898:. New York: Oxford University Press.
330:A star becomes a giant after all the
262:and correspond to luminosity classes
7:
25:
838:can become peculiar blue giants.
798:Blue (and sometimes white) giants
793:(ÎČ Corvi), a G-type bright giant.
2949:
2937:
2925:
2913:
2886:
2876:
2875:
367:), once the core is depleted of
30:
848:(λ Orionis A), an O-type giant.
787:(α Aurigae Aa), a G-type giant.
1201:"The end of the main sequence"
1140:(class notes). Astronomy 534,
864:(α Draconis), an A-type giant.
605:Yerkes spectral classification
424:In stars above about 0.4
256:Yerkes spectral classification
1:
2788:Timeline of stellar astronomy
996:American Institute of Physics
392:SchönbergâChandrasekhar limit
346:depends largely on its mass.
826:, and depending on mass and
571:(Îł Gem), an A-type subgiant;
2448:HertzsprungâRussell diagram
1345:10.1051/0004-6361/200912351
875:List of nearest giant stars
708:(α Boötis), a K-type giant.
583:(ÎŽ Sco), a B-type subgiant.
577:(η Boo), a G-type subgiant.
260:HertzsprungâRussell diagram
228:has a substantially larger
38:HertzsprungâRussell diagram
2993:
2362:KelvinâHelmholtz mechanism
1315:Astronomy and Astrophysics
1092:and P. A. Bradley (1995).
801:
658:
553:
2871:
1625:
1412:
1289:. Springer. p. 176.
1206:The Astrophysical Journal
984:Twentieth Century Physics
29:
2741:With multiple exoplanets
1135:"Giants and Post-Giants"
758:Type I Cepheid variables
1527:Asymptotic giant branch
1337:2009A&A...503..521M
1283:Steven J. Dick (2019).
1242:Abt, Helmut A. (1957).
1119:10.1515/astro-1995-0213
824:asymptotic giant branch
817:horizontal-branch stars
680:asymptotic giant branch
485:Stars in the 8~12
464:asymptotic giant branch
350:Intermediate-mass stars
344:post-main-sequence star
2863:Tidal disruption event
2352:Circumstellar envelope
1586:Luminous blue variable
1371:giant-star comparison.
896:Astronomy Encyclopedia
342:. The behaviour of a
327:
2388:Effective temperature
1248:Astrophysical Journal
1142:Penn State University
764:Delta Scuti variables
702:, a G-type red giant.
629:Epsilon Canis Majoris
319:
2858:Planet-hosting stars
2736:With resolved images
2707:Historical brightest
2637:Photometric-standard
2563:Solar radio emission
2357:Eddington luminosity
2137:Triple-alpha process
2075:ThorneâĆ»ytkow object
1450:Young stellar object
992:Institute of Physics
990:, UK; New York, NY:
834:experiencing a late
752:W Virginis variables
599:of luminosity class
441:triple-alpha process
282:(namely K and M) by
2682:Highest temperature
2453:Colorâcolor diagram
2318:Protoplanetary disk
2122:Protonâproton chain
1800:Chemically peculiar
1260:1957ApJ...126..503A
1219:1997ApJ...482..420L
1186:2004MmSAI..75..694E
1110:1995BaltA...4..166K
961:1914PA.....22..275R
649:Gamma Canis Majoris
439:in the core by the
248:surface temperature
246:) star of the same
2687:Lowest temperature
2438:Photometric system
2408:Absolute magnitude
2342:Circumstellar dust
1955:Stellar black hole
1591:Stellar population
1477:HerbigâHaro object
974:Brown, Laurie M.;
746:RR Lyrae variables
445:begins explosively
328:
2901:
2900:
2804:Substellar object
2783:Planetary nebulae
2202:Luminous red nova
2112:Deuterium burning
2098:
2097:
1581:Instability strip
1561:Wolf-Rayet nebula
1515:Horizontal branch
1460:Pre-main-sequence
1133:Robin Ciardullo.
1028:Jacqueline Mitton
949:Popular Astronomy
738:instability strip
714:, a M-type giant.
696:, a K-type giant.
672:horizontal branch
449:horizontal branch
286:in 1905 or 1906.
284:Ejnar Hertzsprung
16:(Redirected from
2984:
2954:
2953:
2952:
2942:
2941:
2940:
2930:
2929:
2928:
2918:
2917:
2916:
2909:
2893:Stars portal
2891:
2890:
2879:
2878:
2535:Planetary system
2458:Strömgren sphere
2330:Asteroseismology
2051:Black hole star
1623:
1549:Planetary nebula
1510:Red-giant branch
1399:
1392:
1385:
1376:
1356:
1355:
1330:
1310:
1301:
1300:
1280:
1274:
1273:
1271:
1239:
1233:
1232:
1230:
1196:
1190:
1189:
1179:
1177:astro-ph/0409583
1159:
1153:
1152:
1150:
1144:. Archived from
1139:
1130:
1124:
1123:
1121:
1098:Baltic Astronomy
1086:
1080:
1079:
1061:
1046:
1045:
1024:
1018:
1017:
998:. p. 1696.
971:
965:
964:
944:
938:
937:
919:
910:
909:
891:
726:, a K-type giant
700:Epsilon Ophiuchi
668:red-giant branch
519:
400:red-giant branch
219:
202:
195:
188:
181:
174:
167:
160:
153:
146:
137:
130:
123:
116:
109:
102:
95:
88:
81:
74:
67:
60:
53:
46:
39:
34:
21:
2992:
2991:
2987:
2986:
2985:
2983:
2982:
2981:
2962:
2961:
2960:
2950:
2948:
2938:
2936:
2926:
2924:
2914:
2912:
2904:
2902:
2897:
2885:
2867:
2792:
2761:Milky Way novae
2697:Smallest volume
2641:
2622:Radial velocity
2545:
2539:
2491:Common envelope
2467:
2366:
2335:Helioseismology
2306:Bipolar outflow
2247:Microturbulence
2242:Convection zone
2223:
2117:Lithium burning
2104:Nucleosynthesis
2094:
1976:
1885:
1612:
1491:
1440:Molecular cloud
1421:
1408:
1403:
1365:
1360:
1359:
1312:
1311:
1304:
1297:
1282:
1281:
1277:
1241:
1240:
1236:
1198:
1197:
1193:
1161:
1160:
1156:
1148:
1137:
1132:
1131:
1127:
1088:
1087:
1083:
1076:
1063:
1062:
1049:
1042:
1026:
1025:
1021:
1006:
982:, eds. (1995).
973:
972:
968:
946:
945:
941:
934:
921:
920:
913:
906:
893:
892:
888:
883:
871:
806:
800:
733:
663:
657:
590:
569:Gamma Geminorum
558:
552:
544:
530:
527:
517:
511:
508:
503:
491:
488:
480:
477:
472:
470:High-mass stars
460:
457:
430:
427:
412:
409:
389:
386:
365:
362:
352:
314:
222:
221:
217:
213:
211:
209:
207:
204:
200:
197:
193:
190:
186:
183:
179:
176:
172:
169:
165:
162:
158:
155:
151:
148:
144:
142:
139:
135:
132:
128:
125:
121:
118:
114:
111:
107:
104:
100:
97:
93:
90:
86:
83:
79:
76:
72:
69:
65:
62:
58:
55:
51:
48:
44:
41:
37:
28:
23:
22:
15:
12:
11:
5:
2990:
2988:
2980:
2979:
2974:
2964:
2963:
2959:
2958:
2946:
2934:
2922:
2899:
2898:
2896:
2895:
2883:
2872:
2869:
2868:
2866:
2865:
2860:
2855:
2850:
2845:
2840:
2835:
2830:
2829:
2828:
2823:
2822:
2821:
2816:
2800:
2798:
2794:
2793:
2791:
2790:
2785:
2780:
2779:
2778:
2773:
2763:
2758:
2753:
2748:
2743:
2738:
2733:
2732:
2731:
2726:
2725:
2724:
2714:
2709:
2704:
2699:
2694:
2692:Largest volume
2689:
2684:
2679:
2669:
2668:
2667:
2662:
2651:
2649:
2643:
2642:
2640:
2639:
2634:
2629:
2624:
2619:
2618:
2617:
2612:
2607:
2597:
2592:
2587:
2582:
2577:
2576:
2575:
2570:
2565:
2560:
2549:
2547:
2541:
2540:
2538:
2537:
2532:
2531:
2530:
2525:
2520:
2510:
2505:
2504:
2503:
2498:
2493:
2488:
2477:
2475:
2469:
2468:
2466:
2465:
2460:
2455:
2450:
2445:
2440:
2435:
2430:
2425:
2420:
2415:
2410:
2405:
2403:Magnetic field
2400:
2395:
2390:
2385:
2380:
2374:
2372:
2368:
2367:
2365:
2364:
2359:
2354:
2349:
2344:
2339:
2338:
2337:
2327:
2326:
2325:
2320:
2313:Accretion disk
2310:
2309:
2308:
2303:
2293:
2292:
2291:
2289:Alfvén surface
2286:
2284:Stellar corona
2281:
2276:
2271:
2261:
2259:Radiation zone
2256:
2255:
2254:
2249:
2239:
2233:
2231:
2225:
2224:
2222:
2221:
2216:
2215:
2214:
2209:
2204:
2199:
2194:
2184:
2179:
2174:
2169:
2164:
2159:
2154:
2149:
2144:
2139:
2134:
2129:
2124:
2119:
2114:
2108:
2106:
2100:
2099:
2096:
2095:
2093:
2092:
2087:
2082:
2077:
2072:
2067:
2066:
2065:
2060:
2057:
2049:
2048:
2047:
2042:
2037:
2032:
2027:
2022:
2017:
2012:
2007:
1997:
1992:
1986:
1984:
1978:
1977:
1975:
1974:
1969:
1968:
1967:
1957:
1952:
1951:
1950:
1945:
1944:
1943:
1938:
1928:
1918:
1917:
1916:
1906:
1901:
1895:
1893:
1887:
1886:
1884:
1883:
1881:Blue straggler
1878:
1877:
1876:
1866:
1861:
1860:
1859:
1849:
1848:
1847:
1842:
1837:
1832:
1827:
1822:
1817:
1812:
1807:
1797:
1792:
1791:
1790:
1785:
1780:
1770:
1769:
1768:
1758:
1757:
1756:
1751:
1746:
1736:
1731:
1730:
1729:
1724:
1719:
1709:
1704:
1699:
1694:
1693:
1692:
1687:
1677:
1676:
1675:
1670:
1665:
1660:
1655:
1650:
1645:
1639:Main sequence
1637:
1632:
1626:
1620:
1618:Classification
1614:
1613:
1611:
1610:
1609:
1608:
1603:
1593:
1588:
1583:
1578:
1573:
1568:
1563:
1558:
1557:
1556:
1554:Protoplanetary
1546:
1541:
1540:
1539:
1534:
1524:
1523:
1522:
1512:
1507:
1501:
1499:
1493:
1492:
1490:
1489:
1484:
1479:
1474:
1473:
1472:
1467:
1462:
1457:
1447:
1442:
1437:
1431:
1429:
1423:
1422:
1420:
1419:
1413:
1410:
1409:
1404:
1402:
1401:
1394:
1387:
1379:
1373:
1372:
1364:
1363:External links
1361:
1358:
1357:
1321:(2): 521â531,
1302:
1295:
1275:
1269:10.1086/146423
1234:
1228:10.1086/304125
1213:(1): 420â432.
1191:
1154:
1151:on 2011-07-20.
1125:
1104:(2): 166â220.
1081:
1074:
1047:
1040:
1030:, ed. (2001).
1019:
1004:
966:
939:
932:
911:
904:
885:
884:
882:
879:
878:
877:
870:
867:
866:
865:
859:
849:
832:post-AGB stars
802:Main article:
799:
796:
795:
794:
788:
782:
779:Sigma Octantis
768:
767:
761:
755:
749:
732:
729:
728:
727:
721:
715:
709:
703:
697:
684:post-AGB stars
659:Main article:
656:
653:
652:
651:
646:
644:Alpha Herculis
641:
636:
631:
626:
621:
589:
586:
585:
584:
578:
572:
554:Main article:
551:
548:
543:
540:
528:
525:
509:
506:
502:
501:Low-mass stars
499:
489:
486:
478:
475:
471:
468:
458:
455:
428:
425:
410:
407:
387:
384:
363:
360:
351:
348:
334:available for
313:
310:
215:
205:
198:
194:Red supergiant
191:
184:
177:
170:
163:
156:
149:
140:
133:
126:
119:
112:
105:
98:
91:
84:
77:
70:
63:
56:
49:
42:
35:
26:
24:
14:
13:
10:
9:
6:
4:
3:
2:
2989:
2978:
2975:
2973:
2970:
2969:
2967:
2957:
2947:
2945:
2935:
2933:
2923:
2921:
2911:
2907:
2894:
2889:
2884:
2882:
2874:
2873:
2870:
2864:
2861:
2859:
2856:
2854:
2853:Intergalactic
2851:
2849:
2846:
2844:
2841:
2839:
2836:
2834:
2833:Galactic year
2831:
2827:
2824:
2820:
2817:
2815:
2812:
2811:
2810:
2807:
2806:
2805:
2802:
2801:
2799:
2795:
2789:
2786:
2784:
2781:
2777:
2774:
2772:
2769:
2768:
2767:
2764:
2762:
2759:
2757:
2754:
2752:
2749:
2747:
2744:
2742:
2739:
2737:
2734:
2730:
2727:
2723:
2720:
2719:
2718:
2715:
2713:
2712:Most luminous
2710:
2708:
2705:
2703:
2700:
2698:
2695:
2693:
2690:
2688:
2685:
2683:
2680:
2678:
2675:
2674:
2673:
2670:
2666:
2663:
2661:
2658:
2657:
2656:
2653:
2652:
2650:
2648:
2644:
2638:
2635:
2633:
2630:
2628:
2627:Proper motion
2625:
2623:
2620:
2616:
2613:
2611:
2608:
2606:
2603:
2602:
2601:
2598:
2596:
2593:
2591:
2590:Constellation
2588:
2586:
2583:
2581:
2578:
2574:
2571:
2569:
2566:
2564:
2561:
2559:
2558:Solar eclipse
2556:
2555:
2554:
2551:
2550:
2548:
2544:Earth-centric
2542:
2536:
2533:
2529:
2526:
2524:
2521:
2519:
2516:
2515:
2514:
2511:
2509:
2506:
2502:
2499:
2497:
2494:
2492:
2489:
2487:
2484:
2483:
2482:
2479:
2478:
2476:
2474:
2470:
2464:
2461:
2459:
2456:
2454:
2451:
2449:
2446:
2444:
2441:
2439:
2436:
2434:
2431:
2429:
2426:
2424:
2421:
2419:
2416:
2414:
2411:
2409:
2406:
2404:
2401:
2399:
2396:
2394:
2391:
2389:
2386:
2384:
2381:
2379:
2376:
2375:
2373:
2369:
2363:
2360:
2358:
2355:
2353:
2350:
2348:
2345:
2343:
2340:
2336:
2333:
2332:
2331:
2328:
2324:
2321:
2319:
2316:
2315:
2314:
2311:
2307:
2304:
2302:
2299:
2298:
2297:
2294:
2290:
2287:
2285:
2282:
2280:
2277:
2275:
2272:
2270:
2267:
2266:
2265:
2262:
2260:
2257:
2253:
2250:
2248:
2245:
2244:
2243:
2240:
2238:
2235:
2234:
2232:
2230:
2226:
2220:
2217:
2213:
2210:
2208:
2205:
2203:
2200:
2198:
2195:
2193:
2190:
2189:
2188:
2185:
2183:
2180:
2178:
2175:
2173:
2170:
2168:
2165:
2163:
2160:
2158:
2155:
2153:
2150:
2148:
2145:
2143:
2142:Alpha process
2140:
2138:
2135:
2133:
2130:
2128:
2125:
2123:
2120:
2118:
2115:
2113:
2110:
2109:
2107:
2105:
2101:
2091:
2088:
2086:
2083:
2081:
2078:
2076:
2073:
2071:
2068:
2064:
2061:
2058:
2056:
2053:
2052:
2050:
2046:
2043:
2041:
2038:
2036:
2033:
2031:
2028:
2026:
2023:
2021:
2018:
2016:
2013:
2011:
2008:
2006:
2003:
2002:
2001:
1998:
1996:
1993:
1991:
1988:
1987:
1985:
1983:
1979:
1973:
1970:
1966:
1963:
1962:
1961:
1958:
1956:
1953:
1949:
1946:
1942:
1939:
1937:
1934:
1933:
1932:
1929:
1927:
1924:
1923:
1922:
1919:
1915:
1914:Helium planet
1912:
1911:
1910:
1907:
1905:
1904:Parker's star
1902:
1900:
1897:
1896:
1894:
1892:
1888:
1882:
1879:
1875:
1872:
1871:
1870:
1867:
1865:
1862:
1858:
1855:
1854:
1853:
1850:
1846:
1843:
1841:
1838:
1836:
1835:Lambda Boötis
1833:
1831:
1828:
1826:
1823:
1821:
1818:
1816:
1813:
1811:
1808:
1806:
1803:
1802:
1801:
1798:
1796:
1793:
1789:
1786:
1784:
1781:
1779:
1776:
1775:
1774:
1771:
1767:
1764:
1763:
1762:
1759:
1755:
1752:
1750:
1747:
1745:
1742:
1741:
1740:
1737:
1735:
1732:
1728:
1725:
1723:
1720:
1718:
1715:
1714:
1713:
1710:
1708:
1705:
1703:
1700:
1698:
1695:
1691:
1688:
1686:
1683:
1682:
1681:
1678:
1674:
1671:
1669:
1666:
1664:
1661:
1659:
1656:
1654:
1651:
1649:
1646:
1644:
1641:
1640:
1638:
1636:
1633:
1631:
1628:
1627:
1624:
1621:
1619:
1615:
1607:
1604:
1602:
1601:Superluminous
1599:
1598:
1597:
1594:
1592:
1589:
1587:
1584:
1582:
1579:
1577:
1574:
1572:
1569:
1567:
1564:
1562:
1559:
1555:
1552:
1551:
1550:
1547:
1545:
1542:
1538:
1535:
1533:
1530:
1529:
1528:
1525:
1521:
1518:
1517:
1516:
1513:
1511:
1508:
1506:
1505:Main sequence
1503:
1502:
1500:
1498:
1494:
1488:
1485:
1483:
1482:Hayashi track
1480:
1478:
1475:
1471:
1468:
1466:
1463:
1461:
1458:
1456:
1453:
1452:
1451:
1448:
1446:
1443:
1441:
1438:
1436:
1433:
1432:
1430:
1428:
1424:
1418:
1415:
1414:
1411:
1407:
1400:
1395:
1393:
1388:
1386:
1381:
1380:
1377:
1370:
1367:
1366:
1362:
1354:
1350:
1346:
1342:
1338:
1334:
1329:
1324:
1320:
1316:
1309:
1307:
1303:
1298:
1296:9783030103804
1292:
1288:
1287:
1279:
1276:
1270:
1265:
1261:
1257:
1253:
1249:
1245:
1238:
1235:
1229:
1224:
1220:
1216:
1212:
1208:
1207:
1202:
1195:
1192:
1187:
1183:
1178:
1173:
1169:
1165:
1158:
1155:
1147:
1143:
1136:
1129:
1126:
1120:
1115:
1111:
1107:
1103:
1099:
1095:
1091:
1085:
1082:
1077:
1075:0-470-09219-X
1071:
1067:
1060:
1058:
1056:
1054:
1052:
1048:
1043:
1041:0-521-80045-5
1037:
1033:
1029:
1023:
1020:
1015:
1011:
1007:
1005:0-7503-0310-7
1001:
997:
993:
989:
985:
981:
980:Pippard, A.B.
977:
976:Pais, Abraham
970:
967:
962:
958:
954:
950:
943:
940:
935:
933:0-8160-5998-5
929:
925:
918:
916:
912:
907:
905:0-19-521833-7
901:
897:
890:
887:
880:
876:
873:
872:
868:
863:
860:
857:
853:
850:
847:
844:
843:
842:
839:
837:
836:thermal pulse
833:
829:
825:
820:
818:
813:
811:
805:
797:
792:
789:
786:
783:
780:
777:
776:
775:
772:
765:
762:
759:
756:
753:
750:
747:
744:
743:
742:
739:
731:Yellow giants
730:
725:
722:
719:
716:
713:
710:
707:
704:
701:
698:
695:
692:
691:
690:
687:
685:
681:
677:
673:
670:(RGB); a red
669:
662:
654:
650:
647:
645:
642:
640:
639:Beta Draconis
637:
635:
634:Theta Scorpii
632:
630:
627:
625:
622:
620:
617:
616:
615:
612:
610:
606:
602:
598:
594:
593:Bright giants
588:Bright giants
587:
582:
581:Delta Scorpii
579:
576:
573:
570:
567:
566:
565:
562:
557:
549:
547:
541:
539:
537:
534:
523:
515:
500:
498:
494:
483:
469:
467:
465:
452:
450:
446:
442:
438:
434:
422:
420:
416:
404:
401:
397:
393:
382:
379:. The inert
378:
374:
370:
366:
357:
349:
347:
345:
341:
340:main sequence
337:
333:
326:
324:
318:
311:
309:
306:
304:
300:
296:
292:
287:
285:
281:
280:spectral type
277:
273:
269:
265:
261:
257:
253:
249:
245:
244:
239:
238:main-sequence
235:
231:
227:
220:
203:
196:
189:
182:
180:Bright giants
175:
168:
161:
154:
147:
143:Main sequence
138:
131:
124:
117:
110:
103:
96:
89:
82:
75:
68:
61:
54:
47:
45:Spectral type
40:
33:
19:
2956:Solar System
2756:White dwarfs
2746:Brown dwarfs
2729:Most distant
2677:Most massive
2655:Proper names
2615:Photographic
2568:Solar System
2546:observations
2473:Star systems
2296:Stellar wind
2279:Chromosphere
2252:Oscillations
2132:Helium flash
1982:Hypothetical
1960:X-ray binary
1899:Compact star
1734:Bright giant
1711:
1487:Henyey track
1465:Herbig Ae/Be
1318:
1314:
1285:
1278:
1251:
1247:
1237:
1210:
1204:
1194:
1167:
1163:
1157:
1146:the original
1128:
1101:
1097:
1090:S. O. Kepler
1084:
1065:
1031:
1022:
983:
969:
952:
948:
942:
923:
895:
889:
840:
821:
814:
807:
773:
769:
734:
688:
664:
613:
600:
592:
591:
563:
559:
545:
504:
495:
484:
473:
453:
423:
405:
356:solar masses
353:
329:
321:
307:
288:
275:
271:
270:. The terms
267:
263:
251:
241:
223:
157:
122:White dwarfs
115:Brown dwarfs
2977:Giant stars
2944:Outer space
2932:Spaceflight
2809:Brown dwarf
2585:Circumpolar
2463:Kraft break
2443:Color index
2418:Metallicity
2378:Designation
2347:Cosmic dust
2269:Photosphere
2035:Dark-energy
2010:Electroweak
1995:Black dwarf
1926:Radio-quiet
1909:White dwarf
1795:White dwarf
1445:Bok globule
1369:Interactive
955:: 275â294.
828:metallicity
810:blue giants
609:supergiants
536:white dwarf
419:white dwarf
303:hypergiants
299:supergiants
201:Hypergiants
187:Supergiants
173:Blue giants
18:Giant stars
2972:Star types
2966:Categories
2771:Candidates
2766:Supernovae
2751:Red dwarfs
2610:Extinction
2398:Kinematics
2393:Luminosity
2371:Properties
2264:Atmosphere
2162:Si burning
2152:Ne burning
2090:White hole
2063:Quasi-star
1990:Blue dwarf
1845:Technetium
1761:Hypergiant
1739:Supergiant
1032:Giant star
881:References
841:Examples:
804:Blue giant
791:Beta Corvi
785:Capella Aa
774:Examples:
689:Examples:
655:Red giants
575:Eta Bootis
564:Examples:
542:Subclasses
514:convection
234:luminosity
166:Red giants
145:("dwarfs")
129:Red dwarfs
2920:Astronomy
2702:Brightest
2600:Magnitude
2580:Pole star
2501:Symbiotic
2496:Eclipsing
2428:Starlight
2229:Structure
2219:Supernova
2212:Micronova
2207:Recurrent
2192:Symbiotic
2177:p-process
2172:r-process
2167:s-process
2157:O burning
2147:C burning
2127:CNO cycle
2070:Gravastar
1606:Hypernova
1596:Supernova
1571:Dredge-up
1544:Blue loop
1537:super-AGB
1520:Red clump
1497:Evolution
1455:Protostar
1435:Accretion
1427:Formation
1328:0906.3386
724:Aldebaran
712:R Doradus
676:red clump
661:Red giant
550:Subgiants
396:dredge-up
312:Formation
258:) on the
152:Subgiants
136:Subdwarfs
2881:Category
2776:Remnants
2672:Extremes
2632:Parallax
2605:Apparent
2595:Asterism
2573:Sunlight
2523:Globular
2508:Multiple
2433:Variable
2423:Rotation
2383:Dynamics
2274:Starspot
1948:Magnetar
1891:Remnants
1707:Subgiant
1680:Subdwarf
1532:post-AGB
1353:15699426
1014:33102501
869:See also
856:Pleiades
706:Arcturus
556:Subgiant
529:☉
522:Universe
510:☉
490:☉
479:☉
459:☉
429:☉
411:☉
388:☉
377:subgiant
369:hydrogen
364:☉
332:hydrogen
224:A giant
208:absolute
2906:Portals
2848:Gravity
2797:Related
2717:Nearest
2665:Chinese
2513:Cluster
2486:Contact
2323:Proplyd
2197:Remnant
2085:Blitzar
2059:Hawking
2015:Strange
1965:Burster
1921:Neutron
1874:Extreme
1825:He-weak
1470:T Tauri
1333:Bibcode
1256:Bibcode
1254:: 503.
1215:Bibcode
1182:Bibcode
1170:: 694.
1106:Bibcode
988:Bristol
957:Bibcode
852:Alcyone
624:Albireo
619:Canopus
603:in the
254:in the
236:than a
2838:Galaxy
2826:Planet
2814:Desert
2722:bright
2660:Arabic
2481:Binary
2301:Bubble
2025:Planck
2000:Exotic
1936:Binary
1931:Pulsar
1869:Helium
1830:Barium
1773:Carbon
1766:Yellow
1754:Yellow
1727:Yellow
1566:PG1159
1351:
1293:
1072:
1038:
1012:
1002:
930:
902:
862:Thuban
846:Meissa
694:Pollux
678:; the
533:helium
437:oxygen
433:carbon
415:helium
381:helium
336:fusion
325:image.
230:radius
210:magni-
159:Giants
2843:Guest
2647:Lists
2528:Super
2182:Fusor
2055:Black
2040:Quark
2020:Preon
2005:Boson
1941:X-ray
1857:Shell
1810:Ap/Bp
1712:Giant
1630:Early
1576:OH/IR
1406:Stars
1349:S2CID
1323:arXiv
1172:arXiv
1149:(PDF)
1138:(PDF)
924:giant
597:stars
276:dwarf
272:giant
243:dwarf
2518:Open
2413:Mass
2237:Core
2187:Nova
2080:Iron
2030:Dark
1840:Lead
1820:HgMn
1815:CEMP
1744:Blue
1717:Blue
1635:Late
1417:List
1291:ISBN
1070:ISBN
1036:ISBN
1010:OCLC
1000:ISBN
928:ISBN
900:ISBN
718:Mira
595:are
435:and
373:fuse
301:and
274:and
266:and
240:(or
232:and
226:star
212:tude
2819:Sub
2553:Sun
1972:SGR
1749:Red
1722:Red
1341:doi
1319:503
1264:doi
1252:126
1223:doi
1211:482
1114:doi
674:or
323:ESO
295:Sun
291:Sun
268:III
2968::
1852:Be
1805:Am
1788:CH
1783:CN
1702:OB
1697:WR
1347:,
1339:,
1331:,
1317:,
1305:^
1262:.
1250:.
1246:.
1221:.
1209:.
1203:.
1180:.
1168:75
1166:.
1112:.
1100:.
1096:.
1050:^
1008:.
994:,
986:.
978:;
953:22
951:.
914:^
601:II
518:10
451:.
305:.
264:II
214:(M
2908::
2045:Q
1864:B
1778:S
1690:B
1685:O
1673:M
1668:K
1663:G
1658:F
1653:A
1648:B
1643:O
1398:e
1391:t
1384:v
1343::
1335::
1325::
1299:.
1272:.
1266::
1258::
1231:.
1225::
1217::
1188:.
1184::
1174::
1122:.
1116::
1108::
1102:4
1078:.
1044:.
1016:.
963:.
959::
936:.
908:.
858:;
526:M
507:M
487:M
476:M
456:M
426:M
408:M
385:M
361:M
358:(
252:V
218:)
216:V
108:T
101:L
94:M
87:K
80:G
73:F
66:A
59:B
52:O
20:)
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