702:
considered to be a subgiant at this point although there is little change visible from the exterior. As the fusing hydrogen shell converts its mass into helium the convective effect separates the helium towards the core where it very slowly increases the mass of the non-fusing core of nearly pure helium plasma. As this takes place the fusing hydrogen shell gradually expands outward which increases the size of the outer shell of the star up to the subgiant size from two to ten times the original radius of the star when it was on the main sequence. The expansion of the outer layers of the star into the subgiant size nearly balances the increase energy generated by the hydrogen shell fusion causing the star to nearly maintain its surface temperature. This causes the spectral class of the star to change very little in the lower end of this range of star mass. The subgiant surface area radiating the energy is so much larger the potential
1167:) star. The low metallicity star is also over 1,000 K hotter and over twice as luminous at the start of the subgiant branch. The difference in temperature is less pronounced at the end of the subgiant branch, but the low metallicity star is larger and nearly four times as luminous. Similar differences exist in the evolution of stars with other masses, and key values such as the mass of a star that will become a supergiant instead of reaching the red giant branch are lower at low metallicity.
1196:
687:
3843:
28:
769:, but hydrogen shell fusion quickly increases the mass of the core beyond that limit. More-massive stars already have cores above the Schönberg–Chandrasekhar mass when they leave the main sequence. The exact initial mass at which stars will show a hook and at which they will leave the main sequence with cores above the Schönberg–Chandrasekhar limit depend on the metallicity and the degree of
580:
751:
contract and increase in temperature. The entire star contracts and increases in temperature, with the radiated luminosity actually increasing despite the lack of fusion. This continues for several million years before the core becomes hot enough to ignite hydrogen in a shell, which reverses the temperature and luminosity increase and the star starts to expand and cool. This
1176:
3854:
1191:
Subgiants occupy a region above (i.e. more luminous than) the main sequence stars and below the giant stars. There are relatively few on most H–R diagrams because the time spent as a subgiant is much less than the time spent on the main sequence or as a giant star. Hot, class B, subgiants are barely
819:
In very massive O-class main sequence stars, the transition from main sequence to giant to supergiant occurs over a very narrow range of temperature and luminosity, sometimes even before core hydrogen fusion has ended, and the subgiant class is rarely used. Values for the surface gravity, log(g), of
641:
Once a main sequence star ceases to fuse hydrogen in its core, the core begins to collapse under its own weight. This causes it to increase in temperature and hydrogen fuses in a shell outside the core, which provides more energy than core hydrogen burning. Low- and intermediate-mass stars expand and
1207:
Stellar evolutionary tracks can be plotted on an H–R diagram. For a particular mass, these trace the position of a star throughout its life, and show a track from the initial main sequence position, along the subgiant branch, to the giant branch. When an H–R diagram is plotted for a group of stars
1187:
A Hertzsprung–Russell (H–R) diagram is a scatter plot of stars with temperature or spectral type on the x-axis and absolute magnitude or luminosity on the y-axis. H–R diagrams of all stars, show a clear diagonal main sequence band containing the majority of stars, a significant number of red giants
855:
This table shows the typical lifetimes on the main sequence (MS) and subgiant branch (SB), as well as any hook duration between core hydrogen exhaustion and the onset of shell burning, for stars with different initial masses, all at solar metallicity (Z = 0.02). Also shown are the helium core mass,
787:
The core contraction and envelope expansion is very rapid, taking only a few million years. In this time the temperature of the star will cool from its main sequence value of 6,000–30,000 K to around 5,000 K. Relatively few stars are seen in this stage of their evolution and there is an
776:
Once the core exceeds the C–R limit, it can no longer remain in thermal equilibrium with the hydrogen shell. It contracts and the outer layers of the star expand and cool. The energy to expand the outer envelope causes the radiated luminosity to decrease. When the outer layers cool sufficiently,
731:
After one to eight billion years, the helium core becomes too massive to support its own weight and becomes degenerate. Its temperature increases, the rate of fusion in the hydrogen shell increases, the outer layers become strongly convective, and the luminosity increases at approximately the same
570:
Later analysis showed that some of these were blended spectra from double stars and some were variable, and the standards have been expanded to many more stars, but many of the original stars are still considered standards of the subgiant luminosity class. O-class stars and stars cooler than K1 are
626:
both lie in the
Hertzsprung Gap and are likely evolutionary subgiants, but both are often assigned giant luminosity classes. The spectral classification can be influenced by metallicity, rotation, unusual chemical peculiarities, etc. The initial stages of the subgiant branch in a star like the sun
1995:
Carter, Joshua A.; Agol, Eric; Chaplin, William J.; Basu, Sarbani; Bedding, Timothy R.; Buchhave, Lars A.; Christensen-Dalsgaard, Jørgen; Deck, Katherine M.; Elsworth, Yvonne; Fabrycky, Daniel C.; Ford, Eric B.; Fortney, Jonathan J.; Hale, Steven J.; Handberg, Rasmus; Hekker, Saskia (2012-08-03).
286:
Rather than defining absolute features, a typical approach to determining a spectral luminosity class is to compare similar spectra against standard stars. Many line ratios and profiles are sensitive to gravity, and therefore make useful luminosity indicators, but some of the most useful spectral
701:
Stars with 40 percent the mass of the Sun and larger have non-convective cores with a strong temperature gradient from the centre outwards. When they exhaust hydrogen at the core of the star, the shell of hydrogen surrounding the central core continues to fuse without interruption. The star is
664:
are convective throughout most of the star. These stars continue to fuse hydrogen in their cores until essentially the entire star has been converted to helium, and they do not develop into subgiants. Stars of this mass have main-sequence lifetimes many times longer than the current age of the
750:
Stars as massive and larger than the Sun have a convective core on the main sequence. They develop a more massive helium core, taking up a larger fraction of the star, before they exhaust the hydrogen in the entire convective region. Fusion in the star ceases entirely and the core begins to
727:
and it remains in thermal equilibrium with the fusing hydrogen shell. Its mass continues to increase and the star very slowly expands as the hydrogen shell migrates outwards. Any increase in energy output from the shell goes into expanding the envelope of the star and the luminosity stays
2128:
Khandelwal, Akanksha; Sharma, Rishikesh; Chakraborty, Abhijit; Chaturvedi, Priyanka; Ulmer-Moll, Solène; Ciardi, David R.; Boyle, Andrew W.; Baliwal, Sanjay; Bieryla, Allyson; Latham, David W.; Prasad, Neelam J. S. S. V.; Nayak, Ashirbad; Lendl, Monika; Mordasini, Christoph (2023-04-01).
811:
fusion. Hydrogen shell fusion and subsequent core helium fusion begin quickly following core hydrogen exhaustion, before the star could reach the red giant branch. Such stars, for example early B main sequence stars, experience a brief and shortened subgiant branch before becoming
1192:
distinguishable from the main sequence stars, while cooler subgiants fill a relatively large gap between cool main sequence stars and the red giants. Below approximately spectral type K3 the region between the main sequence and red giants is entirely empty, with no subgiants.
777:
they become opaque and force convection to begin outside the fusing shell. The expansion stops and the radiated luminosity begins to increase, which is defined as the start of the red giant branch for these stars. Stars with an initial mass approximately 1–2
1208:
which all have the same age, such as a cluster, the subgiant branch may be visible as a band of stars between the main sequence turnoff point and the red giant branch. The subgiant branch is only visible if the cluster is sufficiently old that 1–8
646:. The transition from the main sequence to the red giant branch is known as the subgiant branch. The shape and duration of the subgiant branch varies for stars of different masses, due to differences in the internal configuration of the star.
856:
surface effective temperature, radius, and luminosity at the start and end of the subgiant branch for each star. The end of the subgiant branch is defined to be when the core becomes degenerate or when the luminosity starts to increase.
627:
are prolonged with little external indication of the internal changes. One approach to identifying evolutionary subgiants include chemical abundances such as
Lithium which is depleted in subgiants, and coronal emission strength.
617:
The subgiant branch is a stage in the evolution of low to intermediate mass stars. Stars with a subgiant spectral type are not always on the evolutionary subgiant branch, and vice versa. For example, the stars
1152:. Low metallicity stars develop a larger helium core before leaving the main sequence, hence lower mass stars show a hook at the start of the subgiant branch. The helium core mass of a Z=0.001 (extreme
706:
where planetary orbits will be in the range to form liquid water is shifted much further out into any planetary system. The surface area of a sphere is found as 4Ď€r so a sphere with a radius of 2
773:
in the convective core. Low metallicity causes the central part of even low mass cores to be convectively unstable, and overshooting causes the core to be larger when hydrogen becomes exhausted.
1235:. ω Centauri actually shows several separate subgiant branches for reasons that are still not fully understood, but appear to represent stellar populations of different ages within the cluster.
279:
to indicate the luminosity relative to other stars of the same temperature. Luminosity class IV stars are the subgiants, located between main-sequence stars (luminosity class V) and
1824:
Pancino, E.; Mucciarelli, A.; Sbordone, L.; Bellazzini, M.; Pasquini, L.; Monaco, L.; Ferraro, F. R. (2011). "The subgiant branch ofω Centauri seen through high-resolution spectroscopy".
2277:
Girardi, L.; Bressan, A.; Bertelli, G.; Chiosi, C. (2000). "Evolutionary tracks and isochrones for low- and intermediate-mass stars: From 0.15 to 7 M?, and from Z=0.0004 to 0.03".
1148:
In general, stars with lower metallicity are smaller and hotter than stars with higher metallicity. For subgiants, this is complicated by different ages and core masses at the
1490:
Lèbre, A.; De
Laverny, P.; De Medeiros, J. R.; Charbonnel, C.; Da Silva, L. (1999). "Lithium and rotation on the subgiant branch. I. Observations and spectral analysis".
1982:
3694:
634:
and so the rate of fusion increases. This causes stars to evolve slowly to higher luminosities as they age and broadens the main sequence band in the
2069:; Chachan, Yayaati; Mawet, Dimitri; Millar-Blanchaer, Maxwell A.; Nilsson, Ricky; Tinyanont, Samaporn; Vasisht, Gautam; Wright, Jason (2020-02-13).
3726:
766:
724:
1644:
Mermilliod, J. C. (1981). "Comparative studies of young open clusters. III – Empirical isochronous curves and the zero age main sequence".
784:
can develop a degenerate helium core before this point and that will cause the star to enter the red giant branch as for lower mass stars.
728:
approximately constant. The subgiant branch for these stars is short, horizontal, and heavily populated, as visible in very old clusters.
275:
system is a two-dimensional scheme that uses a letter and number combination to denote that temperature of a star (e.g. A5 or M1) and a
3701:
3020:
820:
O-class stars are around 3.6 cgs for giants and 3.9 for dwarfs. For comparison, typical log(g) values for K class stars are 1.59 (
393:
Morgan and Keenan listed examples of stars in luminosity class IV when they established the two-dimensional classification scheme:
3413:
635:
32:
3327:
3706:
3343:
2362:
272:
260:
between +2.5 and +4. These were noted as being part of a continuum of stars between obvious main-sequence stars such as the
1300:
while crossing the instability strip, but massive subgiant evolution is very rapid and it is difficult to detect examples.
3753:
3620:
3736:
3687:
3662:
2955:
1344:
Sandage, Allan; Lubin, Lori M.; Vandenberg, Don A. (2003). "The age of the oldest stars in the local galactic disk from
1257:
703:
3040:
1232:
3677:
3657:
1297:
1188:(and white dwarfs if sufficiently faint stars are observed), with relatively few stars in other parts of the diagram.
1785:"WIYN Open Cluster Study. III. The Observed Variation of the Red Clump Luminosity and Color with Metallicity and Age"
1304:
has been proposed as a subgiant on its first crossing but was subsequently determined to be on its second crossing
3741:
3672:
3642:
3748:
3625:
3602:
3184:
2633:
2628:
2623:
2618:
2613:
2608:
1730:
Martins, F.; Schaerer, D.; Hillier, D. J. (2005). "A new calibration of stellar parameters of
Galactic O stars".
1517:
Ayres, Thomas R.; Simon, Theodore; Stern, Robert A.; Drake, Stephen A.; Wood, Brian E.; Brown, Alexander (1998).
2891:
2765:
2400:
3418:
3087:
2065:
Vissapragada, Shreyas; Jontof-Hutter, Daniel; Shporer, Avi; Knutson, Heather A.; Liu, Leo; Thorngren, Daniel;
3884:
3667:
3217:
3127:
3069:
2995:
2566:
2492:
2442:
2130:
3828:
3808:
3580:
3575:
3368:
3317:
3122:
3112:
2785:
2583:
2551:
2425:
2242:
Pols, Onno R.; Schröder, Klaus-Peter; Hurley, Jarrod R.; Tout, Christopher A.; Eggleton, Peter P. (1998).
1603:
Pols, Onno R.; Schröder, Klaus-Peter; Hurley, Jarrod R.; Tout, Christopher A.; Eggleton, Peter P. (1998).
755:
is generally defined as the end of the main sequence and the start of the subgiant branch in these stars.
233:
39:
3682:
3652:
3647:
3637:
3565:
3353:
2519:
2330:
2209:"Evolution of low- and intermediate-mass stars to the end of the asymptotic giant branch with mass loss"
2071:"Diffuser-Assisted Infrared Transit Photometry for Four Dynamically Interacting \textit{Kepler} Systems"
1200:
1149:
375:
2800:
1877:
Ayres, Thomas R. (1984). "A Far-Ultraviolet Study of the Bright Delta Scuti
Variable Beta Cassiopeia".
3823:
3721:
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2015:
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770:
469:
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3423:
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2839:
697:, showing a short but densely-populated subgiant branch of stars slightly less massive than the Sun
3818:
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2005:
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1765:
1739:
1712:
1684:
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1360:
1313:
623:
619:
257:
202:
807:, depending on metallicity, stars have hot massive convective cores on the main sequence due to
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3769:
3254:
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3147:
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2731:
2719:
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1422:
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As the fraction of hydrogen remaining in the core of a main sequence star decreases, the core
399:
245:
2131:"Discovery of a massive giant planet with extreme density around the sub-giant star TOI-4603"
1673:"Comprehensive analytic formulae for stellar evolution as a function of mass and metallicity"
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Long period variables – period luminosity relations and classification in the Gaia
Mission
789:
595:
513:
485:
181:
17:
825:
792:. It is most obvious in clusters from a few hundred million to a few billion years old.
642:
cool until at about 5,000 K they begin to increase in luminosity in a stage known as the
509:
2259:
2224:
2019:
1886:
1800:
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1620:
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3157:
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2714:
2600:
2502:
2392:
2382:
1567:
1220:
1215:
stars have evolved away from the main sequence, which requires several billion years.
833:
816:. They may also be assigned a giant spectral luminosity class during this transition.
631:
523:
489:
479:
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433:
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386:
379:
188:
3873:
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1244:
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1008:
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137:
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3162:
3097:
2980:
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2531:
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2435:
1390:
1224:
1164:
563:
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443:
409:
320:
306:
174:
102:
95:
88:
81:
74:
67:
60:
53:
46:
2165:
1855:
2187:
1996:"Kepler-36: A Pair of Planets with Neighboring Orbits and Dissimilar Densities".
1967:
1942:
1926:
1901:
1761:
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3473:
3446:
3438:
3428:
3408:
3383:
3312:
3234:
2990:
2965:
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2874:
2834:
2795:
2760:
2743:
2738:
2410:
1325:
545:
419:
317:
303:
116:
109:
27:
2097:
2070:
3358:
3055:
3028:
3005:
2985:
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2822:
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2704:
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2541:
1321:
1228:
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813:
579:
557:
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429:
237:
195:
167:
153:
2174:
2106:
2035:
3545:
3393:
3177:
3142:
3137:
3132:
3092:
3045:
3035:
2829:
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2780:
2687:
2638:
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2027:
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821:
808:
713:
will release 400% as much energy at the surface and a sphere with a 10
694:
654:
367:
341:
335:
280:
265:
256:
The term subgiant was first used in 1930 for class G and early K stars with
160:
123:
2043:
268:, although less numerous than either the main sequence or the giant stars.
2308:
1519:"The Coronae of Moderate-Mass Giants in the Hertzsprung Gap and the Clump"
1231:
are sufficiently old that they show a pronounced subgiant branch in their
3538:
3239:
2913:
2645:
2291:
1744:
1689:
1365:
331:
292:
130:
1163:
star at the end of the main sequence is nearly double that of a Z=0.02 (
3813:
3288:
3050:
2817:
2770:
2753:
2748:
2667:
2066:
1411:
An Atlas of
Stellar Spectra, with an Outline of Spectral Classification
495:
359:
349:
1409:
Morgan, William Wilson; Keenan, Philip Childs; Kellman, Edith (1943).
1175:
3803:
3791:
3010:
2896:
1140:
1097:
310:
296:
3853:
2335:
2233:
2208:
2147:
2087:
1809:
1784:
1543:
1518:
1382:
2010:
1838:
1194:
1174:
685:
578:
832:
with log(g) of 3.47. Examples of massive subgiant stars include
16:
This article is about the type of star. For the dance group, see
3172:
3152:
2371:
1203:
and the red giant branch, with a hook at the younger M67 turnoff
610:
lower-mass tracks show very short long-lasting subgiant branches
371:
345:
327:
225:
2344:
1943:"On the crossing mode of the long-period Cepheid SV Vulpeculae"
1671:
Hurley, Jarrod R.; Pols, Onno R.; Tout, Christopher A. (2000).
1426:
23:
Type of star larger than main-sequence but smaller than a giant
3518:
1983:"Astronomers Take a Picture of a Planet Orbiting Another Star"
1054:
261:
240:. The term subgiant is applied both to a particular spectral
828:), leaving plenty of scope to classify subgiants such as
2340:
1900:
Luck, R. E.; Kovtyukh, V. V.; Andrievsky, S. M. (2001).
1199:
Old open clusters showing a subgiant branch between the
1353:
1465:
Bulletin d'Information du Centre de Données
Stellaires
594:
track shows a hook and a subgiant branch crossing the
1266:, late A and early F main sequence and subgiant stars
3762:
3611:
3509:
3437:
3336:
3193:
3068:
2946:
2855:
2582:
2461:
2391:
2331:
Post-main sequence evolution through helium burning
1292:range, this includes Delta Scuti variables such as
1566:
1463:Garcia, B. (1989). "A list of MK standard stars".
2248:Monthly Notices of the Royal Astronomical Society
2244:"Stellar evolution models for Z = 0.0001 to 0.03"
1677:Monthly Notices of the Royal Astronomical Society
1609:Monthly Notices of the Royal Astronomical Society
1605:"Stellar evolution models for Z = 0.0001 to 0.03"
840:, both class O stars with masses of over 20
607:track shows a hook and pronounced subgiant branch
1440:Gray, Richard O.; Corbally, Christopher (2009).
1281:since they may cross the strip again later on a
1260:, mid to late B main sequence and subgiant stars
1312:Planets in orbit around subgiant stars include
1296:. At higher masses the stars would pulsate as
732:effective temperature. The star is now on the
1270:Subgiants more massive than the sun cross the
788:apparent lack in the H–R diagram known as the
2356:
1560:
1558:
1556:
1554:
385:M: strength of the 422.6 nm Ca line and
8:
2279:Astronomy and Astrophysics Supplement Series
1568:"Evolution of Stars and Stellar Populations"
1413:. Chicago, IL: University of Chicago Press.
299:absorption, strong emission is more luminous
2588:
2363:
2349:
2341:
1902:"SV Vulpeculae: A first crossing Cepheid?"
1573:Evolution of Stars and Stellar Populations
1565:Salaris, Maurizio; Cassisi, Santi (2005).
1254:, early B main sequence and subgiant stars
571:rarely given subgiant luminosity classes.
2290:
2267:
2232:
2164:
2146:
2096:
2086:
2009:
1966:
1925:
1837:
1808:
1743:
1706:
1688:
1628:
1542:
1364:
1941:Turner, D. G.; Berdnikov, L. N. (2004).
858:
1336:
348:line strengths, and wing widths in the
1598:
1596:
1594:
1592:
1590:
287:features for each spectral class are:
2207:Vassiliadis, E.; Wood, P. R. (1993).
758:The core of stars below about 2
7:
1404:
1402:
1400:
720:will release 10000% as much energy.
323:, broader wings means less luminous
723:The helium core mass is below the
14:
3852:
3842:
3841:
2269:10.1046/j.1365-8711.1998.01658.x
1708:10.1046/j.1365-8711.2000.03426.x
1630:10.1046/j.1365-8711.1998.01658.x
264:and obvious giant stars such as
26:
2192:Extrasolar Planet Encyclopaedia
1442:Stellar Spectral Classification
228:that is brighter than a normal
1444:. Princeton University Press.
273:Yerkes spectral classification
1:
3754:Timeline of stellar astronomy
1258:Slowly pulsating B-type stars
767:Schönberg–Chandrasekhar limit
725:Schönberg–Chandrasekhar limit
283:(luminosity class III).
2135:Astronomy & Astrophysics
1826:Astronomy & Astrophysics
1171:Subgiants in the H–R diagram
836:and the primary star of the
704:circumstellar habitable zone
583:Stellar evolutionary tracks:
3414:Hertzsprung–Russell diagram
2166:10.1051/0004-6361/202245608
1856:10.1051/0004-6361/201016024
1298:Classical Cepheid variables
636:Hertzsprung–Russell diagram
34:Hertzsprung–Russell diagram
3901:
3328:Kelvin–Helmholtz mechanism
1968:10.1051/0004-6361:20040163
1947:Astronomy and Astrophysics
1927:10.1051/0004-6361:20010615
1906:Astronomy and Astrophysics
1762:10.1051/0004-6361:20042386
1732:Astronomy and Astrophysics
1646:Astronomy and Astrophysics
1492:Astronomy and Astrophysics
1179:H–R diagram of the entire
252:Yerkes luminosity class IV
15:
3837:
2591:
2378:
1523:The Astrophysical Journal
890:
887:
884:
879:
876:
873:
861:
25:
3707:With multiple exoplanets
2098:10.3847/1538-3881/ab65c8
2075:The Astronomical Journal
1789:The Astronomical Journal
1783:Sarajedini, Ata (1999).
1233:color–magnitude diagrams
291:O: relative strength of
236:, but not as bright as
2493:Asymptotic giant branch
2301:2000A&AS..141..371G
2157:2023A&A...672L...7K
2028:10.1126/science.1223269
1959:2004A&A...423..335T
1918:2001A&A...373..589L
1848:2011A&A...527A..18P
1754:2005A&A...436.1049M
1658:1981A&A....97..235M
1504:1999A&A...345..936L
1351:of G and K subgiants".
800:Beyond about 8–12
3829:Tidal disruption event
3318:Circumstellar envelope
2552:Luminous blue variable
2194:. Accessed 1 Feb. 2018
1985:. Accessed 1 Feb. 2018
1879:IUE Proposal ID #DSGTA
1204:
1184:
698:
614:
364:H, and K line profiles
244:and to a stage in the
3354:Effective temperature
2213:Astrophysical Journal
1264:Delta Scuti variables
1252:Beta Cephei variables
1201:main sequence turnoff
1198:
1178:
1150:main sequence turnoff
689:
632:temperature increases
582:
326:F: line strengths of
3824:Planet-hosting stars
3702:With resolved images
3673:Historical brightest
3603:Photometric-standard
3529:Solar radio emission
3323:Eddington luminosity
3103:Triple-alpha process
3041:Thorne–Żytkow object
2416:Young stellar object
2188:"Planet HD 224693 b"
1285:. In the 2 – 3
657:than about 0.4
3648:Highest temperature
3419:Color–color diagram
3284:Protoplanetary disk
3088:Proton–proton chain
2766:Chemically peculiar
2309:10.1051/aas:2000126
2260:1998MNRAS.298..525P
2225:1993ApJ...413..641V
2020:2012Sci...337..556C
1887:1984iue..prop.1747A
1801:1999AJ....118.2321S
1699:2000MNRAS.315..543H
1621:1998MNRAS.298..525P
1581:2005essp.book.....S
1535:1998ApJ...496..428A
1477:1989BICDS..36...27G
1450:2009ssc..book.....G
1419:1943assw.book.....M
1375:2003PASP..115.1187S
1247:include subgiants:
765:is still below the
650:Very-low-mass stars
258:absolute magnitudes
246:evolution of a star
3653:Lowest temperature
3404:Photometric system
3374:Absolute magnitude
3308:Circumstellar dust
2921:Stellar black hole
2557:Stellar population
2443:Herbig–Haro object
1359:(812): 1187–1206.
1314:Kappa Andromedae b
1205:
1185:
699:
655:Stars less massive
615:
309:, and strength of
3867:
3866:
3770:Substellar object
3749:Planetary nebulae
3168:Luminous red nova
3078:Deuterium burning
3064:
3063:
2547:Instability strip
2527:Wolf-Rayet nebula
2481:Horizontal branch
2426:Pre-main-sequence
2004:(6094): 556–559.
1275:instability strip
1243:Several types of
1217:Globular clusters
1146:
1145:
740:Mass 1 to 8
374:line ratios, and
232:star of the same
3892:
3859:Stars portal
3857:
3856:
3845:
3844:
3501:Planetary system
3424:Strömgren sphere
3296:Asteroseismology
3017:Black hole star
2589:
2515:Planetary nebula
2476:Red-giant branch
2365:
2358:
2351:
2342:
2320:
2294:
2292:astro-ph/9910164
2273:
2271:
2238:
2236:
2195:
2185:
2179:
2178:
2168:
2150:
2125:
2119:
2118:
2100:
2090:
2062:
2056:
2055:
2013:
1992:
1986:
1979:
1973:
1972:
1970:
1938:
1932:
1931:
1929:
1897:
1891:
1890:
1874:
1868:
1867:
1841:
1821:
1815:
1814:
1812:
1795:(5): 2321–2326.
1780:
1774:
1773:
1747:
1745:astro-ph/0503346
1738:(3): 1049–1065.
1727:
1721:
1720:
1710:
1692:
1690:astro-ph/0001295
1668:
1662:
1661:
1641:
1635:
1634:
1632:
1600:
1585:
1584:
1570:
1562:
1549:
1548:
1546:
1514:
1508:
1507:
1487:
1481:
1480:
1460:
1454:
1453:
1437:
1431:
1430:
1406:
1395:
1394:
1368:
1366:astro-ph/0307128
1341:
1011:
859:
838:δ Circini system
734:Red-giant branch
692:globular cluster
690:H–R diagram for
644:red-giant branch
242:luminosity class
215:
198:
191:
184:
177:
170:
163:
156:
149:
142:
133:
126:
119:
112:
105:
98:
91:
84:
77:
70:
63:
56:
49:
42:
35:
30:
3900:
3899:
3895:
3894:
3893:
3891:
3890:
3889:
3870:
3869:
3868:
3863:
3851:
3833:
3758:
3727:Milky Way novae
3663:Smallest volume
3607:
3588:Radial velocity
3511:
3505:
3457:Common envelope
3433:
3332:
3301:Helioseismology
3272:Bipolar outflow
3213:Microturbulence
3208:Convection zone
3189:
3083:Lithium burning
3070:Nucleosynthesis
3060:
2942:
2851:
2578:
2457:
2406:Molecular cloud
2387:
2374:
2369:
2327:
2276:
2241:
2206:
2203:
2198:
2186:
2182:
2127:
2126:
2122:
2064:
2063:
2059:
1994:
1993:
1989:
1980:
1976:
1940:
1939:
1935:
1899:
1898:
1894:
1876:
1875:
1871:
1823:
1822:
1818:
1782:
1781:
1777:
1729:
1728:
1724:
1670:
1669:
1665:
1643:
1642:
1638:
1602:
1601:
1588:
1564:
1563:
1552:
1516:
1515:
1511:
1489:
1488:
1484:
1462:
1461:
1457:
1439:
1438:
1434:
1408:
1407:
1398:
1343:
1342:
1338:
1334:
1310:
1291:
1288:
1241:
1214:
1211:
1173:
1162:
1159:
1009:
966:
963:
956:
953:
946:
939:
936:
929:
926:
919:
916:
909:
902:
899:
881:
870:
867:
863:
853:
846:
843:
806:
803:
798:
790:Hertzsprung gap
783:
780:
764:
761:
748:
746:
743:
719:
716:
712:
709:
684:
682:
679:
675:
672:
663:
660:
652:
613:
606:
603:
596:Hertzsprung gap
593:
590:
577:
575:Subgiant branch
568:
470:λ Ursae Majoris
254:
218:
217:
213:
209:
207:
205:
203:
200:
196:
193:
189:
186:
182:
179:
175:
172:
168:
165:
161:
158:
154:
151:
147:
144:
140:
138:
135:
131:
128:
124:
121:
117:
114:
110:
107:
103:
100:
96:
93:
89:
86:
82:
79:
75:
72:
68:
65:
61:
58:
54:
51:
47:
44:
40:
37:
33:
24:
21:
18:Subgiant (band)
12:
11:
5:
3898:
3896:
3888:
3887:
3885:Subgiant stars
3882:
3872:
3871:
3865:
3864:
3862:
3861:
3849:
3838:
3835:
3834:
3832:
3831:
3826:
3821:
3816:
3811:
3806:
3801:
3796:
3795:
3794:
3789:
3788:
3787:
3782:
3766:
3764:
3760:
3759:
3757:
3756:
3751:
3746:
3745:
3744:
3739:
3729:
3724:
3719:
3714:
3709:
3704:
3699:
3698:
3697:
3692:
3691:
3690:
3680:
3675:
3670:
3665:
3660:
3658:Largest volume
3655:
3650:
3645:
3635:
3634:
3633:
3628:
3617:
3615:
3609:
3608:
3606:
3605:
3600:
3595:
3590:
3585:
3584:
3583:
3578:
3573:
3563:
3558:
3553:
3548:
3543:
3542:
3541:
3536:
3531:
3526:
3515:
3513:
3507:
3506:
3504:
3503:
3498:
3497:
3496:
3491:
3486:
3476:
3471:
3470:
3469:
3464:
3459:
3454:
3443:
3441:
3435:
3434:
3432:
3431:
3426:
3421:
3416:
3411:
3406:
3401:
3396:
3391:
3386:
3381:
3376:
3371:
3369:Magnetic field
3366:
3361:
3356:
3351:
3346:
3340:
3338:
3334:
3333:
3331:
3330:
3325:
3320:
3315:
3310:
3305:
3304:
3303:
3293:
3292:
3291:
3286:
3279:Accretion disk
3276:
3275:
3274:
3269:
3259:
3258:
3257:
3255:Alfvén surface
3252:
3250:Stellar corona
3247:
3242:
3237:
3227:
3225:Radiation zone
3222:
3221:
3220:
3215:
3205:
3199:
3197:
3191:
3190:
3188:
3187:
3182:
3181:
3180:
3175:
3170:
3165:
3160:
3150:
3145:
3140:
3135:
3130:
3125:
3120:
3115:
3110:
3105:
3100:
3095:
3090:
3085:
3080:
3074:
3072:
3066:
3065:
3062:
3061:
3059:
3058:
3053:
3048:
3043:
3038:
3033:
3032:
3031:
3026:
3023:
3015:
3014:
3013:
3008:
3003:
2998:
2993:
2988:
2983:
2978:
2973:
2963:
2958:
2952:
2950:
2944:
2943:
2941:
2940:
2935:
2934:
2933:
2923:
2918:
2917:
2916:
2911:
2910:
2909:
2904:
2894:
2884:
2883:
2882:
2872:
2867:
2861:
2859:
2853:
2852:
2850:
2849:
2847:Blue straggler
2844:
2843:
2842:
2832:
2827:
2826:
2825:
2815:
2814:
2813:
2808:
2803:
2798:
2793:
2788:
2783:
2778:
2773:
2763:
2758:
2757:
2756:
2751:
2746:
2736:
2735:
2734:
2724:
2723:
2722:
2717:
2712:
2702:
2697:
2696:
2695:
2690:
2685:
2675:
2670:
2665:
2660:
2659:
2658:
2653:
2643:
2642:
2641:
2636:
2631:
2626:
2621:
2616:
2611:
2605:Main sequence
2603:
2598:
2592:
2586:
2584:Classification
2580:
2579:
2577:
2576:
2575:
2574:
2569:
2559:
2554:
2549:
2544:
2539:
2534:
2529:
2524:
2523:
2522:
2520:Protoplanetary
2512:
2507:
2506:
2505:
2500:
2490:
2489:
2488:
2478:
2473:
2467:
2465:
2459:
2458:
2456:
2455:
2450:
2445:
2440:
2439:
2438:
2433:
2428:
2423:
2413:
2408:
2403:
2397:
2395:
2389:
2388:
2386:
2385:
2379:
2376:
2375:
2370:
2368:
2367:
2360:
2353:
2345:
2339:
2338:
2333:
2326:
2325:External links
2323:
2322:
2321:
2285:(3): 371–383.
2274:
2239:
2234:10.1086/173033
2202:
2199:
2197:
2196:
2180:
2120:
2057:
1987:
1974:
1933:
1892:
1869:
1816:
1810:10.1086/301112
1775:
1722:
1663:
1636:
1586:
1550:
1544:10.1086/305347
1529:(1): 428–448.
1509:
1482:
1455:
1432:
1396:
1383:10.1086/378243
1335:
1333:
1330:
1309:
1306:
1289:
1286:
1279:first crossing
1268:
1267:
1261:
1255:
1240:
1237:
1212:
1209:
1172:
1169:
1160:
1157:
1144:
1143:
1138:
1135:
1132:
1129:
1126:
1123:
1120:
1117:
1114:
1111:
1108:
1105:
1101:
1100:
1095:
1092:
1089:
1086:
1083:
1080:
1077:
1074:
1071:
1068:
1065:
1062:
1058:
1057:
1051:
1048:
1045:
1042:
1039:
1036:
1033:
1030:
1027:
1024:
1021:
1018:
1014:
1013:
1006:
1003:
1000:
997:
994:
991:
988:
985:
982:
979:
976:
973:
969:
968:
964:
961:
958:
954:
951:
948:
944:
941:
937:
934:
931:
927:
924:
921:
917:
914:
911:
907:
904:
900:
897:
893:
892:
889:
886:
883:
878:
875:
872:
868:
865:
852:
849:
844:
841:
804:
801:
797:
794:
781:
778:
762:
759:
747:
744:
741:
738:
717:
714:
710:
707:
683:
680:
677:
673:
670:
667:
661:
658:
651:
648:
612:
611:
608:
604:
601:
598:
591:
588:
584:
576:
573:
567:
566:
560:
554:
548:
542:
536:
526:
516:
502:
492:
482:
476:
462:
456:
450:
440:
422:
412:
406:
395:
391:
390:
383:
382:line strengths
356:
338:
324:
314:
300:
253:
250:
234:spectral class
211:
201:
194:
190:Red supergiant
187:
180:
173:
166:
159:
152:
145:
136:
129:
122:
115:
108:
101:
94:
87:
80:
73:
66:
59:
52:
45:
38:
31:
22:
13:
10:
9:
6:
4:
3:
2:
3897:
3886:
3883:
3881:
3878:
3877:
3875:
3860:
3855:
3850:
3848:
3840:
3839:
3836:
3830:
3827:
3825:
3822:
3820:
3819:Intergalactic
3817:
3815:
3812:
3810:
3807:
3805:
3802:
3800:
3799:Galactic year
3797:
3793:
3790:
3786:
3783:
3781:
3778:
3777:
3776:
3773:
3772:
3771:
3768:
3767:
3765:
3761:
3755:
3752:
3750:
3747:
3743:
3740:
3738:
3735:
3734:
3733:
3730:
3728:
3725:
3723:
3720:
3718:
3715:
3713:
3710:
3708:
3705:
3703:
3700:
3696:
3693:
3689:
3686:
3685:
3684:
3681:
3679:
3678:Most luminous
3676:
3674:
3671:
3669:
3666:
3664:
3661:
3659:
3656:
3654:
3651:
3649:
3646:
3644:
3641:
3640:
3639:
3636:
3632:
3629:
3627:
3624:
3623:
3622:
3619:
3618:
3616:
3614:
3610:
3604:
3601:
3599:
3596:
3594:
3593:Proper motion
3591:
3589:
3586:
3582:
3579:
3577:
3574:
3572:
3569:
3568:
3567:
3564:
3562:
3559:
3557:
3556:Constellation
3554:
3552:
3549:
3547:
3544:
3540:
3537:
3535:
3532:
3530:
3527:
3525:
3524:Solar eclipse
3522:
3521:
3520:
3517:
3516:
3514:
3510:Earth-centric
3508:
3502:
3499:
3495:
3492:
3490:
3487:
3485:
3482:
3481:
3480:
3477:
3475:
3472:
3468:
3465:
3463:
3460:
3458:
3455:
3453:
3450:
3449:
3448:
3445:
3444:
3442:
3440:
3436:
3430:
3427:
3425:
3422:
3420:
3417:
3415:
3412:
3410:
3407:
3405:
3402:
3400:
3397:
3395:
3392:
3390:
3387:
3385:
3382:
3380:
3377:
3375:
3372:
3370:
3367:
3365:
3362:
3360:
3357:
3355:
3352:
3350:
3347:
3345:
3342:
3341:
3339:
3335:
3329:
3326:
3324:
3321:
3319:
3316:
3314:
3311:
3309:
3306:
3302:
3299:
3298:
3297:
3294:
3290:
3287:
3285:
3282:
3281:
3280:
3277:
3273:
3270:
3268:
3265:
3264:
3263:
3260:
3256:
3253:
3251:
3248:
3246:
3243:
3241:
3238:
3236:
3233:
3232:
3231:
3228:
3226:
3223:
3219:
3216:
3214:
3211:
3210:
3209:
3206:
3204:
3201:
3200:
3198:
3196:
3192:
3186:
3183:
3179:
3176:
3174:
3171:
3169:
3166:
3164:
3161:
3159:
3156:
3155:
3154:
3151:
3149:
3146:
3144:
3141:
3139:
3136:
3134:
3131:
3129:
3126:
3124:
3121:
3119:
3116:
3114:
3111:
3109:
3108:Alpha process
3106:
3104:
3101:
3099:
3096:
3094:
3091:
3089:
3086:
3084:
3081:
3079:
3076:
3075:
3073:
3071:
3067:
3057:
3054:
3052:
3049:
3047:
3044:
3042:
3039:
3037:
3034:
3030:
3027:
3024:
3022:
3019:
3018:
3016:
3012:
3009:
3007:
3004:
3002:
2999:
2997:
2994:
2992:
2989:
2987:
2984:
2982:
2979:
2977:
2974:
2972:
2969:
2968:
2967:
2964:
2962:
2959:
2957:
2954:
2953:
2951:
2949:
2945:
2939:
2936:
2932:
2929:
2928:
2927:
2924:
2922:
2919:
2915:
2912:
2908:
2905:
2903:
2900:
2899:
2898:
2895:
2893:
2890:
2889:
2888:
2885:
2881:
2880:Helium planet
2878:
2877:
2876:
2873:
2871:
2870:Parker's star
2868:
2866:
2863:
2862:
2860:
2858:
2854:
2848:
2845:
2841:
2838:
2837:
2836:
2833:
2831:
2828:
2824:
2821:
2820:
2819:
2816:
2812:
2809:
2807:
2804:
2802:
2801:Lambda Boötis
2799:
2797:
2794:
2792:
2789:
2787:
2784:
2782:
2779:
2777:
2774:
2772:
2769:
2768:
2767:
2764:
2762:
2759:
2755:
2752:
2750:
2747:
2745:
2742:
2741:
2740:
2737:
2733:
2730:
2729:
2728:
2725:
2721:
2718:
2716:
2713:
2711:
2708:
2707:
2706:
2703:
2701:
2698:
2694:
2691:
2689:
2686:
2684:
2681:
2680:
2679:
2676:
2674:
2671:
2669:
2666:
2664:
2661:
2657:
2654:
2652:
2649:
2648:
2647:
2644:
2640:
2637:
2635:
2632:
2630:
2627:
2625:
2622:
2620:
2617:
2615:
2612:
2610:
2607:
2606:
2604:
2602:
2599:
2597:
2594:
2593:
2590:
2587:
2585:
2581:
2573:
2570:
2568:
2567:Superluminous
2565:
2564:
2563:
2560:
2558:
2555:
2553:
2550:
2548:
2545:
2543:
2540:
2538:
2535:
2533:
2530:
2528:
2525:
2521:
2518:
2517:
2516:
2513:
2511:
2508:
2504:
2501:
2499:
2496:
2495:
2494:
2491:
2487:
2484:
2483:
2482:
2479:
2477:
2474:
2472:
2471:Main sequence
2469:
2468:
2466:
2464:
2460:
2454:
2451:
2449:
2448:Hayashi track
2446:
2444:
2441:
2437:
2434:
2432:
2429:
2427:
2424:
2422:
2419:
2418:
2417:
2414:
2412:
2409:
2407:
2404:
2402:
2399:
2398:
2396:
2394:
2390:
2384:
2381:
2380:
2377:
2373:
2366:
2361:
2359:
2354:
2352:
2347:
2346:
2343:
2337:
2334:
2332:
2329:
2328:
2324:
2318:
2314:
2310:
2306:
2302:
2298:
2293:
2288:
2284:
2280:
2275:
2270:
2265:
2261:
2257:
2253:
2249:
2245:
2240:
2235:
2230:
2226:
2222:
2218:
2214:
2210:
2205:
2204:
2200:
2193:
2189:
2184:
2181:
2176:
2172:
2167:
2162:
2158:
2154:
2149:
2144:
2140:
2136:
2132:
2124:
2121:
2116:
2112:
2108:
2104:
2099:
2094:
2089:
2084:
2080:
2076:
2072:
2068:
2061:
2058:
2053:
2049:
2045:
2041:
2037:
2033:
2029:
2025:
2021:
2017:
2012:
2007:
2003:
1999:
1991:
1988:
1984:
1981:Plait, Phil.
1978:
1975:
1969:
1964:
1960:
1956:
1952:
1948:
1944:
1937:
1934:
1928:
1923:
1919:
1915:
1911:
1907:
1903:
1896:
1893:
1888:
1884:
1880:
1873:
1870:
1865:
1861:
1857:
1853:
1849:
1845:
1840:
1835:
1831:
1827:
1820:
1817:
1811:
1806:
1802:
1798:
1794:
1790:
1786:
1779:
1776:
1771:
1767:
1763:
1759:
1755:
1751:
1746:
1741:
1737:
1733:
1726:
1723:
1718:
1714:
1709:
1704:
1700:
1696:
1691:
1686:
1682:
1678:
1674:
1667:
1664:
1659:
1655:
1651:
1647:
1640:
1637:
1631:
1626:
1622:
1618:
1614:
1610:
1606:
1599:
1597:
1595:
1593:
1591:
1587:
1582:
1578:
1574:
1569:
1561:
1559:
1557:
1555:
1551:
1545:
1540:
1536:
1532:
1528:
1524:
1520:
1513:
1510:
1505:
1501:
1497:
1493:
1486:
1483:
1478:
1474:
1470:
1466:
1459:
1456:
1451:
1447:
1443:
1436:
1433:
1428:
1424:
1420:
1416:
1412:
1405:
1403:
1401:
1397:
1392:
1388:
1384:
1380:
1376:
1372:
1367:
1362:
1358:
1354:
1350:
1347:
1340:
1337:
1331:
1329:
1327:
1323:
1319:
1315:
1307:
1305:
1303:
1302:SV Vulpeculae
1299:
1295:
1284:
1280:
1277:, called the
1276:
1273:
1265:
1262:
1259:
1256:
1253:
1250:
1249:
1248:
1246:
1245:variable star
1238:
1236:
1234:
1230:
1226:
1225:open clusters
1222:
1218:
1202:
1197:
1193:
1189:
1182:
1177:
1170:
1168:
1166:
1155:
1154:population II
1151:
1142:
1139:
1136:
1133:
1130:
1127:
1124:
1121:
1118:
1115:
1112:
1109:
1106:
1103:
1102:
1099:
1096:
1093:
1090:
1087:
1084:
1081:
1078:
1075:
1072:
1069:
1066:
1063:
1060:
1059:
1056:
1052:
1049:
1046:
1043:
1040:
1037:
1034:
1031:
1028:
1025:
1022:
1019:
1016:
1015:
1012:
1010:Lacaille 8760
1007:
1004:
1001:
998:
995:
992:
989:
986:
983:
980:
977:
974:
971:
970:
959:
949:
942:
932:
922:
912:
905:
895:
894:
860:
857:
850:
848:
839:
835:
831:
827:
823:
817:
815:
810:
796:Massive stars
795:
793:
791:
785:
774:
772:
768:
756:
754:
739:
737:
735:
729:
726:
721:
705:
696:
693:
688:
668:
666:
656:
649:
647:
645:
639:
637:
633:
628:
625:
621:
609:
599:
597:
586:
585:
581:
574:
572:
565:
561:
559:
555:
553:
549:
547:
543:
541:
537:
535:
531:
527:
525:
521:
520:50 Andromedae
517:
515:
511:
507:
503:
501:
497:
493:
491:
487:
483:
481:
477:
475:
471:
467:
463:
461:
457:
455:
451:
449:
448:ζ Cassiopeiae
445:
441:
439:
435:
431:
427:
423:
421:
417:
413:
411:
407:
405:
401:
400:Îł Cassiopeiae
397:
396:
394:
388:
384:
381:
377:
373:
369:
365:
361:
357:
355:
354:H and K lines
351:
347:
343:
339:
337:
333:
329:
325:
322:
321:line profiles
319:
315:
312:
308:
305:
301:
298:
295:emission and
294:
290:
289:
288:
284:
282:
278:
277:Roman numeral
274:
269:
267:
263:
259:
251:
249:
247:
243:
239:
235:
231:
230:main-sequence
227:
223:
216:
199:
192:
185:
178:
176:Bright giants
171:
164:
157:
150:
143:
139:Main sequence
134:
127:
120:
113:
106:
99:
92:
85:
78:
71:
64:
57:
50:
43:
41:Spectral type
36:
29:
19:
3722:White dwarfs
3712:Brown dwarfs
3695:Most distant
3643:Most massive
3621:Proper names
3581:Photographic
3534:Solar System
3512:observations
3439:Star systems
3262:Stellar wind
3245:Chromosphere
3218:Oscillations
3098:Helium flash
2948:Hypothetical
2926:X-ray binary
2865:Compact star
2700:Bright giant
2672:
2453:Henyey track
2431:Herbig Ae/Be
2282:
2278:
2251:
2247:
2216:
2212:
2201:Bibliography
2191:
2183:
2138:
2134:
2123:
2078:
2074:
2060:
2001:
1997:
1990:
1977:
1950:
1946:
1936:
1909:
1905:
1895:
1878:
1872:
1829:
1825:
1819:
1792:
1788:
1778:
1735:
1731:
1725:
1680:
1676:
1666:
1649:
1645:
1639:
1612:
1608:
1572:
1526:
1522:
1512:
1495:
1491:
1485:
1468:
1464:
1458:
1441:
1435:
1410:
1356:
1352:
1348:
1345:
1339:
1311:
1278:
1269:
1242:
1206:
1190:
1186:
1165:population I
1147:
960:Luminosity (
923:Luminosity (
854:
826:α Centauri B
824:) and 4.37 (
818:
799:
786:
775:
771:overshooting
757:
752:
749:
730:
722:
700:
676:to 0.9
653:
640:
629:
616:
569:
500:110 Herculis
392:
285:
270:
255:
221:
219:
146:
118:White dwarfs
111:Brown dwarfs
3775:Brown dwarf
3551:Circumpolar
3429:Kraft break
3409:Color index
3384:Metallicity
3344:Designation
3313:Cosmic dust
3235:Photosphere
3001:Dark-energy
2976:Electroweak
2961:Black dwarf
2892:Radio-quiet
2875:White dwarf
2761:White dwarf
2411:Bok globule
2067:Lee, Eve J.
1953:: 335–340.
1326:HD 224693 b
1239:Variability
877:Hook (MYrs)
834:θ Orionis A
814:supergiants
600:the 2
587:the 5
514:Îł Serpentis
490:ζ Serpentis
486:δ Geminorum
474:β Serpentis
304:Balmer line
238:giant stars
197:Hypergiants
183:Supergiants
169:Blue giants
3880:Star types
3874:Categories
3737:Candidates
3732:Supernovae
3717:Red dwarfs
3576:Extinction
3364:Kinematics
3359:Luminosity
3337:Properties
3230:Atmosphere
3128:Si burning
3118:Ne burning
3056:White hole
3029:Quasi-star
2956:Blue dwarf
2811:Technetium
2727:Hypergiant
2705:Supergiant
2254:(2): 525.
2148:2303.11841
2088:1907.04445
2081:(3): 108.
1912:(2): 589.
1683:(3): 543.
1615:(2): 525.
1349:Parallaxes
1332:References
1322:TOI-4603 b
1221:ω Centauri
851:Properties
665:Universe.
546:ÎĽ Herculis
534:ζ Herculis
524:θ Draconis
480:δ Herculis
460:Ď„ Herculis
454:Îą Herculis
434:θ Ophiuchi
281:red giants
162:Red giants
141:("dwarfs")
125:Red dwarfs
3668:Brightest
3566:Magnitude
3546:Pole star
3467:Symbiotic
3462:Eclipsing
3394:Starlight
3195:Structure
3185:Supernova
3178:Micronova
3173:Recurrent
3158:Symbiotic
3143:p-process
3138:r-process
3133:s-process
3123:O burning
3113:C burning
3093:CNO cycle
3036:Gravastar
2572:Hypernova
2562:Supernova
2537:Dredge-up
2510:Blue loop
2503:super-AGB
2486:Red clump
2463:Evolution
2421:Protostar
2401:Accretion
2393:Formation
2175:0004-6361
2115:195874295
2107:1538-3881
2036:0036-8075
2011:1206.4718
1839:1012.4756
1346:Hipparcos
1320:b and c,
1318:Kepler-36
1283:blue loop
1181:Hipparcos
1156:) 1
933:He Core (
896:He Core (
874:MS (GYrs)
822:Aldebaran
809:CNO cycle
669:0.4
552:β Aquilae
466:β Aurigae
438:λ Scorpii
430:Ď€ Scorpii
426:Îł Orionis
410:β Scorpii
404:δ Scorpii
266:Aldebaran
148:Subgiants
132:Subdwarfs
3847:Category
3742:Remnants
3638:Extremes
3598:Parallax
3571:Apparent
3561:Asterism
3539:Sunlight
3489:Globular
3474:Multiple
3399:Variable
3389:Rotation
3349:Dynamics
3240:Starspot
2914:Magnetar
2857:Remnants
2673:Subgiant
2646:Subdwarf
2498:post-AGB
2317:14566232
2052:40245894
2044:22722249
1881:: 1747.
1864:54951859
1770:39162419
1717:18523597
1290:☉
1227:such as
1223:and old
1219:such as
1213:☉
1161:☉
965:☉
955:☉
950:Radius (
938:☉
928:☉
918:☉
913:Radius (
901:☉
891:Example
869:☉
845:☉
830:η Cephei
805:☉
782:☉
763:☉
745:☉
718:☉
711:☉
681:☉
674:☉
662:☉
605:☉
592:☉
564:Îł Cephei
558:η Cephei
540:ÎĽ Cancri
530:η Boötis
510:θ Boötis
506:τ Boötis
444:Îł Pegasi
420:β Cephei
416:Îż Persei
307:profiles
222:subgiant
204:absolute
3814:Gravity
3763:Related
3683:Nearest
3631:Chinese
3479:Cluster
3452:Contact
3289:Proplyd
3163:Remnant
3051:Blitzar
3025:Hawking
2981:Strange
2931:Burster
2887:Neutron
2840:Extreme
2791:He-weak
2436:T Tauri
2297:Bibcode
2256:Bibcode
2221:Bibcode
2219:: 641.
2153:Bibcode
2016:Bibcode
1998:Science
1955:Bibcode
1914:Bibcode
1883:Bibcode
1844:Bibcode
1832:: A18.
1797:Bibcode
1750:Bibcode
1695:Bibcode
1654:Bibcode
1652:: 235.
1617:Bibcode
1577:Bibcode
1575:: 400.
1531:Bibcode
1500:Bibcode
1498:: 936.
1473:Bibcode
1446:Bibcode
1427:43-2093
1415:Bibcode
1391:7159325
1371:Bibcode
1308:Planets
1272:Cepheid
1183:catalog
1125:1,571.4
496:Procyon
3804:Galaxy
3792:Planet
3780:Desert
3688:bright
3626:Arabic
3447:Binary
3267:Bubble
2991:Planck
2966:Exotic
2902:Binary
2897:Pulsar
2835:Helium
2796:Barium
2739:Carbon
2732:Yellow
2720:Yellow
2693:Yellow
2532:PG1159
2315:
2173:
2141:: L7.
2113:
2105:
2050:
2042:
2034:
1862:
1768:
1715:
1471:: 27.
1425:
1389:
1141:Alkaid
1119:14,544
1098:Sirius
882:(MYrs)
624:31 Com
620:FK Com
442:B2.5:
408:B0.5:
334:, and
318:Balmer
206:magni-
155:Giants
3809:Guest
3613:Lists
3494:Super
3148:Fusor
3021:Black
3006:Quark
2986:Preon
2971:Boson
2907:X-ray
2823:Shell
2776:Ap/Bp
2678:Giant
2596:Early
2542:OH/IR
2372:Stars
2313:S2CID
2287:arXiv
2143:arXiv
2111:S2CID
2083:arXiv
2048:S2CID
2006:arXiv
1860:S2CID
1834:arXiv
1766:S2CID
1740:arXiv
1713:S2CID
1685:arXiv
1387:S2CID
1361:arXiv
1294:β Cas
1137:866.0
1131:4,737
1116:0.806
1088:5,220
1076:7,490
1073:0.240
1044:5,034
1032:5,766
1029:0.025
1026:2,600
999:4,634
987:4,763
984:0.047
981:5,100
885:Start
389:bands
313:lines
224:is a
3484:Open
3379:Mass
3203:Core
3153:Nova
3046:Iron
2996:Dark
2806:Lead
2786:HgMn
2781:CEMP
2710:Blue
2683:Blue
2601:Late
2383:List
2171:ISSN
2103:ISSN
2040:PMID
2032:ISSN
1423:LCCN
1324:and
1134:43.8
1128:0.83
1094:19.6
1085:0.25
1082:36.6
1053:The
1041:0.13
996:0.10
975:58.8
862:Mass
753:hook
622:and
562:K1:
556:K0:
550:G8:
544:G5:
538:G2:
528:G0:
518:F8:
504:F6:
494:F5:
484:F2:
478:A3:
464:A2:
458:B5:
452:B3:
424:B2:
414:B1:
398:B0:
378:and
344:and
271:The
226:star
208:tude
3785:Sub
3519:Sun
2938:SGR
2715:Red
2688:Red
2305:doi
2283:141
2264:doi
2252:298
2229:doi
2217:413
2161:doi
2139:672
2093:doi
2079:159
2024:doi
2002:337
1963:doi
1951:423
1922:doi
1910:373
1852:doi
1830:527
1805:doi
1793:118
1758:doi
1736:436
1703:doi
1681:315
1625:doi
1613:298
1539:doi
1527:496
1496:345
1379:doi
1357:115
1229:M67
1122:6.3
1110:0.4
1107:0.1
1104:5.0
1091:5.4
1079:3.6
1064:1.2
1061:2.0
1055:Sun
1050:2.2
1047:2.0
1038:1.5
1035:1.2
1023:N/A
1020:9.3
1017:1.0
1005:0.6
1002:1.2
993:0.3
990:0.9
978:N/A
972:0.6
947:(K)
945:eff
910:(K)
908:eff
888:End
387:TiO
380:TiO
376:MgH
358:K:
340:G:
316:A:
302:B:
262:Sun
3876::
2818:Be
2771:Am
2754:CH
2749:CN
2668:OB
2663:WR
2311:.
2303:.
2295:.
2281:.
2262:.
2250:.
2246:.
2227:.
2215:.
2211:.
2190:,
2169:.
2159:.
2151:.
2137:.
2133:.
2109:.
2101:.
2091:.
2077:.
2073:.
2046:.
2038:.
2030:.
2022:.
2014:.
2000:.
1961:.
1949:.
1945:.
1920:.
1908:.
1904:.
1858:.
1850:.
1842:.
1828:.
1803:.
1791:.
1787:.
1764:.
1756:.
1748:.
1734:.
1711:.
1701:.
1693:.
1679:.
1675:.
1650:97
1648:.
1623:.
1611:.
1607:.
1589:^
1571:.
1553:^
1537:.
1525:.
1521:.
1494:.
1469:36
1467:.
1421:.
1399:^
1385:.
1377:.
1369:.
1355:.
1328:.
1316:,
1113:15
1070:22
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