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682:'strikes'. At the dimmest part of a Cepheid's cycle, this ionized gas in the outer layers of the star is relatively opaque, and so is heated by the star's radiation, and due to the increasing temperature, begins to expand. As it expands, it cools, but remains ionised until another threshold is reached at which point double ionization cannot be sustained and the layer becomes singly ionized hence more transparent, which allows radiation to escape. The expansion then stops, and reverses due to the star's gravitational attraction. The star's states are held to be either expanding or contracting by the
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597:(established from Classical Cepheids) ranging between 60 km/s/Mpc and 80 km/s/Mpc. Resolving this discrepancy is one of the foremost problems in astronomy since the cosmological parameters of the Universe may be constrained by supplying a precise value of the Hubble constant. Uncertainties have diminished over the years, due in part to discoveries such as
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354:(but still brighter than RR Lyrae stars). Baade's seminal discovery led to a twofold increase in the distance to M31, and the extragalactic distance scale. RR Lyrae stars, then known as Cluster Variables, were recognized fairly early as being a separate class of variable, due in part to their short periods.
3224:
Benedict, G. Fritz; McArthur, B. E.; Fredrick, L. W.; Harrison, T. E.; Slesnick, C. L.; Rhee, J.; Patterson, R. J.; Skrutskie, M. F.; Franz, O. G.; Wasserman, L. H.; Jefferys, W. H.; Nelan, E.; Van Altena, W.; Shelus, P. J.; Hemenway, P. D.; Duncombe, R. L.; Story, D.; Whipple, A. L.; Bradley, A. J.
2620:
Soszyński, I.; Udalski, A.; Szymański, M. K.; Kubiak, M.; Pietrzyński, G.; Wyrzykowski, Ł.; Szewczyk, O.; Ulaczyk, K.; Poleski, R. (2008). "The
Optical Gravitational Lensing Experiment. The OGLE-III Catalog of Variable Stars. II.Type II Cepheids and Anomalous Cepheids in the Large Magellanic Cloud".
2218:
Soszyński, I.; Udalski, A.; Szymański, M. K.; Kubiak, M.; Pietrzyński, G.; Wyrzykowski, Ł.; Szewczyk, O.; Ulaczyk, K.; Poleski, R. (2008). "The
Optical Gravitational Lensing Experiment. The OGLE-III Catalog of Variable Stars. II.Type II Cepheids and Anomalous Cepheids in the Large Magellanic Cloud".
183:
helium, the form adopted at high temperatures, is more opaque than singly ionized helium. As a result, the outer layer of the star cycles between being compressed, which heats the helium until it becomes doubly ionized and (due to opacity) absorbs enough heat to expand; and expanded, which cools the
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recognized two separate populations of
Cepheids (classical and type II). Classical Cepheids are younger and more massive population I stars, whereas type II Cepheids are older, fainter Population II stars. Classical Cepheids and type II Cepheids follow different period-luminosity relationships. The
1875:
Freedman, Wendy L.; Madore, Barry F.; Gibson, Brad K.; Ferrarese, Laura; Kelson, Daniel D.; Sakai, Shoko; Mould, Jeremy R.; Kennicutt, Jr., Robert C.; Ford, Holland C.; Graham, John A.; Huchra, John P.; Hughes, Shaun M. G.; Illingworth, Garth D.; Macri, Lucas M.; Stetson, Peter B. (2001). "Final
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A group of pulsating stars on the instability strip have periods of less than 2 days, similar to RR Lyrae variables but with higher luminosities. Anomalous
Cepheid variables have masses higher than type II Cepheids, RR Lyrae variables, and the Sun. It is unclear whether they are young stars on a
247:
a few months later. The number of similar variables grew to several dozen by the end of the 19th century, and they were referred to as a class as
Cepheids. Most of the Cepheids were known from the distinctive light curve shapes with the rapid increase in brightness and a hump, but some with more
2739:
Benedict, G. Fritz; McArthur, Barbara E.; Feast, Michael W.; Barnes, Thomas G.; Harrison, Thomas E.; Patterson, Richard J.; Menzies, John W.; Bean, Jacob L.; Freedman, Wendy L. (2007). "Hubble Space
Telescope Fine Guidance Sensor Parallaxes of Galactic Cepheid Variable Stars: Period-Luminosity
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helium (helium whose atoms are missing both electrons) is more opaque than singly ionized helium. As helium is heated, its temperature rises until it reaches the point at which double ionisation spontaneously occurs and is sustained throughout the layer in much the same way a fluorescent tube
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A small proportion of
Cepheid variables have been observed to pulsate in two modes at the same time, usually the fundamental and first overtone, occasionally the second overtone. A very small number pulsate in three modes, or an unusual combination of modes including higher overtones.
2816:
Udalski, A.; Wyrzykowski, L.; Pietrzynski, G.; Szewczyk, O.; Szymanski, M.; Kubiak, M.; Soszynski, I.; Zebrun, K. (2001). "The
Optical Gravitational Lensing Experiment. Cepheids in the Galaxy IC1613: No Dependence of the Period-Luminosity Relation on Metallicity".
2699:
Soszynski, I.; Poleski, R.; Udalski, A.; Kubiak, M.; Szymanski, M. K.; Pietrzynski, G.; Wyrzykowski, L.; Szewczyk, O.; Ulaczyk, K. (2008). "The
Optical Gravitational Lensing Experiment. Triple-Mode and 1O/3O Double-Mode Cepheids in the Large Magellanic Cloud".
1723:
1112:"A series of observations on, and a discovery of, the period of the variation of the light of the star marked δ by Bayer, near the head of Cepheus. In a letter from John Goodricke, Esq. to Nevil Maskelyne, D.D.F.R.S. and Astronomer Royal"
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distance measurements to
Cepheid variables and other bodies within 7,500 light-years is vastly improved by comparing images from Hubble taken six months apart, from opposite points in the Earth's orbit. (Between two such observations 2
842:
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Bono, G.; Caputo, F.; Fiorentino, G.; Marconi, M.; Musella, I. (2008). "Cepheids in External Galaxies. I. The Maser-Host Galaxy NGC 4258 and the Metallicity Dependence of Period-Luminosity and Period-Wesenheit Relations".
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attempted to find distances to 13 Cepheids using their motion through the sky. (His results would later require revision.) In 1918, Harlow Shapley used Cepheids to place initial constraints on the size and shape of the
2463:
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Riess, Adam G.; Casertano, Stefano; Anderson, Jay; MacKenty, John; Filippenko, Alexei V. (2014). "Parallax beyond a Kiloparsec from Spatially Scanning the Wide Field Camera 3 on the Hubble Space Telescope".
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can be established. Classical Cepheids have also been used to clarify many characteristics of the Milky Way galaxy, such as the Sun's height above the galactic plane and the Galaxy's local spiral structure.
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Classical Cepheids (also known as Population I Cepheids, type I Cepheids, or Delta Cepheid variables) undergo pulsations with very regular periods on the order of days to months. Classical Cepheids are
2795:
Stanek, K. Z.; Udalski, A. (1999). "The Optical Gravitational Lensing Experiment. Investigating the Influence of Blending on the Cepheid Distance Scale with Cepheids in the Large Magellanic Cloud".
686:
generated by the doubly ionized helium and indefinitely flip-flops between the two states reversing every time the upper or lower threshold is crossed. This process is rather analogous to the
345:
In the mid 20th century, significant problems with the astronomical distance scale were resolved by dividing the Cepheids into different classes with very different properties. In the 1940s,
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of a Cepheid by observing its pulsation period. This in turn gives the distance to the star by comparing its known luminosity to its observed brightness, calibrated by directly observing the
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helium until it becomes singly ionized and (due to transparency) cools and collapses again. Cepheid variables become dimmest during the part of the cycle when the helium is doubly ionized.
1231:
1116:
740:
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Macri, L. M.; Stanek, K. Z.; Bersier, D.; Greenhill, L. J.; Reid, M. J. (2006). "A New Cepheid Distance to the Maser-Host Galaxy NGC 4258 and Its Implications for the Hubble Constant".
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511:-poor, old (~10 Gyr), low mass objects (~half the mass of the Sun). Type II Cepheids are divided into several subgroups by period. Stars with periods between 1 and 4 days are of the
879:
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Shapley, Harlow. (1918). "No. 153. Studies based on the colors and magnitudes in stellar clusters. Eighth paper: The luminosities and distances of 139 Cepheid variables".
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Matsunaga, Noriyuki; Fukushi, Hinako; Nakada, Yoshikazu; Tanabé, Toshihiko; Feast, Michael W.; Menzies, John W.; Ita, Yoshifusa; Nishiyama, Shogo; et al. (2006).
1365:
Hertzsprung, E. (1913). "Über die räumliche Verteilung der Veränderlichen vom δ Cephei-Typus" [On the spatial distribution of variable of the δ Cephei type].
2124:. Stellar Pulsation: Challenges for Theory and Observation: Proceedings of the International Conference. AIP Conference Proceedings. Vol. 1170. pp. 23–25.
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405:. Delta Scuti variables and RR Lyrae variables are not generally treated with Cepheid variables although their pulsations originate with the same helium ionisation
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1655:
Shapley, Harlow (1918). "Studies based on the colors and magnitudes in stellar clusters. Eighth paper: The luminosities and distances of 139 Cepheid variables".
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on both the zero-point and slope of those relations, and the effects of photometric contamination (blending with other stars) and a changing (typically unknown)
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Ngeow, C.; Kanbur, S. M. (2006). "The Hubble Constant from Type Ia Supernovae Calibrated with the Linear and Nonlinear Cepheid Period-Luminosity Relations".
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Macri, Lucas M.; Riess, Adam G.; Guzik, Joyce Ann; Bradley, Paul A. (2009). "The SH0ES Project: Observations of Cepheids in NGC 4258 and Type Ia SN Hosts".
2002:
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Lemaître, G. (1927). "Un Univers homogène de masse constante et de rayon croissant rendant compte de la vitesse radiale des nébuleuses extra-galactiques".
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of the Cepheid period-luminosity relation since its distance is among the most precisely established for a Cepheid, partly because it is a member of a
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Chief among the uncertainties tied to the classical and type II Cepheid distance scale are: the nature of the period-luminosity relation in various
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which are 4–20 times more massive than the Sun, and up to 100,000 times more luminous. These Cepheids are yellow bright giants and supergiants of
3114:
De Zeeuw, P. T.; Hoogerwerf, R.; De Bruijne, J. H. J.; Brown, A. G. A.; Blaauw, A. (1999). "A HIPPARCOS Census of the Nearby OB Associations".
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variation with the same period as the luminosity variation, and initially this was interpreted as evidence that these stars were part of a
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demonstrated that this idea should be abandoned. Two years later, Shapley and others had discovered that Cepheid variables changed their
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where k is a proportionality constant. Now, since the surface gravity is related to the sphere mass and radius through the relation:
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1016:
653:
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Majaess, D.; Turner, D.; Gieren, W. (2012). "New Evidence Supporting Cluster Membership for the Keystone Calibrator Delta Cephei".
706:
175:, which occurs when opacity in a star increases with temperature rather than decreasing. The main gas involved is thought to be
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Gorynya, N. A.; Samus, N. N.; Rastorguev, A. S.; Sachkov, M. E. (1996). "A spectroscopic study of the pulsating star BL Her".
2258:
Kubiak, M.; Udalski, A. (2003). "The Optical Gravitational Lensing Experiment. Population II Cepheids in the Galactic Bulge".
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light curves are often separated out as Small Amplitude Cepheids or s-Cepheids, many of them pulsating in the first overtone.
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Cepheid variables are divided into two subclasses which exhibit markedly different masses, ages, and evolutionary histories:
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Time lapse of the Cepheid type variable star Polaris illustrating the visual appearance of its cycle of brightness changes.
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303:" and showed that those variables were not members of the Milky Way. Hubble's finding settled the question raised in the "
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239:, the first known representative of the class of classical Cepheid variables. The eponymous star for classical Cepheids,
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3713:
851:
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The Secret Lives of Cepheids: A Multi-Wavelength Study of the Atmospheres and Real-Time Evolution of Classical Cepheids
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Caputo, F.; Castellani, V.; Degl'Innocenti, S.; Fiorentino, G.; Marconi, M. (2004). "Bright metal-poor variables: Why
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4116:
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418:
382:
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3225:(2002). "Astrometry with the Hubble Space Telescope: A Parallax of the Fundamental Distance Calibrator δ Cephei".
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Turner, David G. (2010). "The PL calibration for Milky Way Cepheids and its implications for the distance scale".
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Leavitt, Henrietta S.; Pickering, Edward C. (1912). "Periods of 25 variable stars in the Small Magellanic Cloud".
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Madore, Barry F.; Freedman, Wendy L. (2009). "Concerning the Slope of the Cepheid Period-Luminosity Relation".
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697:(1826–1908) demonstrated that the adiabatic radial pulsation period for a homogeneous sphere is related to its
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31:
434:, the prototype of classical cepheids, showing the regular variations produced by intrinsic stellar pulsations
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Feast, Michael W.; Laney, Clifton D.; Kinman, Thomas D.; Van Leeuwen, Floor; Whitelock, Patricia A. (2008).
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variable stars which pulsate with periods typically between 1 and 50 days. Type II Cepheids are typically
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Majaess, D. J. (2010). "RR Lyrae and Type II Cepheid Variables Adhere to a Common Distance Relation".
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A relationship between the period and luminosity for classical Cepheids was discovered in 1908 by
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125:, varying in both diameter and temperature. It changes in brightness, with a well-defined stable
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Majaess, D.; Turner, D.; Lane, D. (2009). "Type II Cepheids as Extragalactic Distance Candles".
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Plachy, E.; et al. (2020), "TESS observations of Cepheid stars: first light results",
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The accepted explanation for the pulsation of Cepheids is called the Eddington valve, or "
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326:'s measurements of the speed at which those galaxies recede from us. They discovered that
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1940:
Tammann, G. A.; Sandage, A.; Reindl, B. (2008). "The expansion field: the value of H 0".
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luminosity of type II Cepheids is, on average, less than classical Cepheids by about 1.5
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263:. She published it in 1912 with further evidence. Cepheid variables were found to show
249:
244:
205:
3314:
3202:
3075:
Majaess, D. (2010). "The Cepheids of Centaurus A (NGC 5128) and Implications for H0".
37:
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4058:
3741:
3611:
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3023:
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307:" of whether the Milky Way represented the entire Universe or was merely one of many
300:
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118:
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David Dunlap Observatory of Toronto University: Galactic Classical Cepheids database
3476:
3322:
3266:
3155:
3008:
2897:
2781:
2660:
Smolec, R.; Moskalik, P. (2008). "Double-Mode Classical Cepheid Models, Revisited".
2606:
2547:
2405:
2344:
2201:
2101:
2041:
1981:
4182:
3965:
3828:
2953:
1328:
Shapley, H. (1916), "The variations in spectral type of twenty Cepheid variables",
917:
905:
609:
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law on Cepheid distances. All these topics are actively debated in the literature.
440:
431:
292:
240:
197:
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365:(who wrote at length on the dynamics of Cepheids), but it was not until 1953 that
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3376:
2598:
4140:
4098:
3435:
Szabados, L.; Kiss, L. L.; Derekas, A. (2007). "The anomalous Cepheid XZ Ceti".
2360:"The luminosities and distance scales of type II Cepheid and RR Lyrae variables"
932:
897:
583:
508:
458:
427:
236:
3547:
3522:
1566:
Baade, W. (1958). "Problems in the determination of the distance of galaxies".
1521:
Wallerstein, George (2002). "The Cepheids of Population II and Related Stars".
3950:
3908:
1973:
1807:
1008:
924:
909:
683:
678:
470:
138:
3361:
1857:
1830:
671:", where the Greek letter κ (kappa) is the usual symbol for the gas opacity.
3985:
3979:
617:
598:
288:
126:
45:
41:
1742:
Turner, David G. (1996). "The Progenitors of Classical Cepheid Variables".
1605:"Section 2: The Great Debate and the Great Mistake: Shapley, Hubble, Baade"
1138:
1088:
341:
Illustration of Cepheid variables (red dots) at the center of the Milky Way
2299:"The period-luminosity relation for type II Cepheids in globular clusters"
1495:
457:
Classical Cepheids are used to determine distances to galaxies within the
3451:
3241:
3130:
3024:"The effect of metallicity on Cepheid magnitudes and the distance to M33"
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2833:
2801:
2756:
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2317:
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1211:
625:
579:
535:
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have short periods and lie on the instability strip where it crosses the
2502:"Period-luminosity relations for type II Cepheids and their application"
913:
165:
17:
2137:
1692:
Eddington, A. S. (1917). "The pulsation theory of Cepheid variables".
393:
are A-type stars on or near the main sequence at the lower end of the
4079:
837:{\displaystyle g=k'{\frac {M}{R^{2}}}=k'{\frac {RM}{R^{3}}}=k'R\rho }
674:
634:
308:
176:
3570:
2000:
Freedman, Wendy L.; Madore, Barry F. (2010). "The Hubble Constant".
248:
symmetrical light curves were known as Geminids after the prototype
148:
This characteristic of classical Cepheids was discovered in 1908 by
129:
and amplitude. Cepheids are important cosmic benchmarks for scaling
4177:
4135:
3504:
3258:
3147:
2945:
2889:
2773:
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1913:
1678:
1589:
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1395:
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1313:
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3297:
3185:
3091:
3042:
2983:
2928:
2716:
2676:
2637:
2520:
2477:
2464:
The Journal of the American Association of Variable Star Observers
2438:
2378:
2235:
2174:
2016:
1956:
1790:
652:
486:
422:
336:
215:
36:
3580:
2500:
Matsunaga, Noriyuki; Feast, Michael W.; Menzies, John W. (2009).
967:
Smith, D. H. (1984). "Eddington's Valve and Cepheid Pulsations".
3960:
3584:
593:
These unresolved matters have resulted in cited values for the
295:
established the distance to classical Cepheid variables in the
3022:
Scowcroft, V.; Bersier, D.; Mould, J. R.; Wood, P. R. (2009).
1065:
Pigott, Edward (1785). "Observations of a new variable star".
450:
F6 – K2 and their radii change by (~25% for the longer-period
103:
3548:
McMaster Cepheid Photometry and Radial Velocity Data Archive
1396:"Globular Clusters and the Structure of the Galactic System"
677:
is the gas thought to be most active in the process. Doubly
519:, and stars with periods greater than 20 days belong to the
3338:"On the existence of hysteresis effects in pulsating stars"
1831:"Radius variation and population type of cepheid variables"
612:
and the availability of precise parallaxes observed by the
526:
Type II Cepheids are used to establish the distance to the
109:
82:
76:
44:, one of the brightest known Cepheid variable stars in the
503:
Type II Cepheids (also termed Population II Cepheids) are
259:
in an investigation of thousands of variable stars in the
1232:
Annals of the Astronomical Observatory of Harvard College
1117:
Philosophical Transactions of the Royal Society of London
88:
3552:
1040:. Astronomy and astrophysics library. Springer. p.
469:
A group of classical Cepheids with small amplitudes and
322:
by combining Cepheid distances to several galaxies with
208:
in 1784. It was the first of its type to be identified.
1524:
Publications of the Astronomical Society of the Pacific
1401:
Publications of the Astronomical Society of the Pacific
633:
apart, a star at a distance of 7500 light-years = 2300
164:
distance to the closest Cepheids such as RS Puppis and
3336:
Auvergne, M.; Baglin, A.; Morel, P. -J. (1981-12-01).
4154:
2156:"Characteristics of the Galaxy according to Cepheids"
1935:
1933:
1931:
854:
752:
709:
106:
100:
79:
73:
3375:
Maurizio Salaris; Santi Cassisi (13 December 2005).
1437:
Hubble, E. P. (1925). "Cepheids in spiral nebulae".
291:
and of the placement of the Sun within it. In 1924,
91:
4097:
4067:
4046:
4030:
4023:
3936:
3901:
3875:
3840:
3797:
3790:
3760:
3732:
3694:
3627:
3618:
2154:Majaess, D. J.; Turner, D. G.; Lane, D. J. (2009).
1745:
Journal of the Royal Astronomical Society of Canada
999:"American Association of Variable Star Observers".
604:Delta Cephei is also of particular importance as a
454:) millions of kilometers during a pulsation cycle.
397:and were originally referred to as dwarf Cepheids.
97:
70:
2507:Monthly Notices of the Royal Astronomical Society
1036:Physics, formation and evolution of rotating stars
873:
836:
734:
152:after studying thousands of variable stars in the
3029:Monthly Notices of the Royal Astronomical Society
2365:Monthly Notices of the Royal Astronomical Society
2304:Monthly Notices of the Royal Astronomical Society
2161:Monthly Notices of the Royal Astronomical Society
2115:
2113:
2111:
1836:Monthly Notices of the Royal Astronomical Society
1516:
1514:
1512:
3553:American Association of Variable Star Observers
2417:
2415:
1995:
1993:
1991:
1870:
1868:
1629:Contributions from the Mount Wilson Observatory
1469:Annales de la Société Scientifique de Bruxelles
1068:Philosophical Transactions of the Royal Society
2149:
2147:
1721:Zhevakin, S. A. (1953). "К Теории Цефеид. I".
1289:"On the Nature and Cause of Cepheid Variation"
1001:The Encyclopedia of Astronomy and Astrophysics
887:is a constant, called the pulsation constant.
30:"Cepheid" redirects here. For other uses, see
3596:
1880:Key Project to Measure the Hubble Constant".
8:
2055:
2053:
2051:
1496:"VISTA Discovers New Component of Milky Way"
27:Type of variable star that pulsates radially
3492:The Astrophysical Journal Supplement Series
2003:Annual Review of Astronomy and Astrophysics
1769:
1767:
735:{\displaystyle T=k\,{\sqrt {\frac {R}{g}}}}
85:
4027:
3794:
3624:
3603:
3589:
3581:
3378:Evolution of Stars and Stellar Populations
3521:
3503:
3450:
3296:
3240:
3184:
3129:
3090:
3059:
3041:
2982:
2927:
2871:
2832:
2800:
2755:
2715:
2675:
2636:
2580:
2537:
2519:
2476:
2437:
2395:
2377:
2334:
2316:
2273:
2234:
2191:
2173:
2075:
2015:
1955:
1895:
1856:
1789:
1421:
1349:
1312:
1227:"1777 variables in the Magellanic Clouds"
1193:
1137:
858:
853:
809:
795:
776:
767:
751:
720:
719:
708:
461:and beyond, and are a means by which the
361:as a heat-engine was proposed in 1917 by
3567:Optical Gravitational Lensing Experiment
495:, a Type II cepheid, recorded by NASA's
4161:
2213:
2211:
956:
171:Cepheids change brightness due to the
1943:The Astronomy and Astrophysics Review
1609:The Cepheid Distance Scale: A History
555:in binary systems, or a mix of both.
497:Transiting Exoplanet Survey Satellite
299:, until then known as the "Andromeda
7:
1261:Harvard College Observatory Circular
994:
992:
962:
960:
645:limit of the available telescopes.)
137:exists between a Cepheid variable's
131:galactic and extragalactic distances
2034:10.1146/annurev-astro-082708-101829
243:, was discovered to be variable by
874:{\displaystyle T{\sqrt {\rho }}=Q}
641:arc-seconds = 2 x 10 degrees, the
637:would appear to move an angle of /
624:space telescopes. The accuracy of
179:. The cycle is driven by the fact
25:
1287:Shapley, Harlow (December 1914).
701:and radius through the relation:
547:"turned-back" horizontal branch,
4188:
4176:
4164:
4134:
3061:10.1111/j.1365-2966.2009.14822.x
2539:10.1111/j.1365-2966.2009.14992.x
2397:10.1111/j.1365-2966.2008.13181.x
2336:10.1111/j.1365-2966.2006.10620.x
2193:10.1111/j.1365-2966.2009.15096.x
318:formulated what is now known as
220:The period-luminosity curves of
156:. The discovery establishes the
66:
369:identified ionized helium as a
3571:Variable Stars catalog website
1777:Astrophysics and Space Science
1225:Leavitt, Henrietta S. (1908).
942:(overtone pulsation mode) and
1:
3724:Blue large-amplitude pulsator
330:, confirming the theories of
3001:10.1088/0004-637X/696/2/1498
938:Anomalous Cepheids include:
896:Classical Cepheids include:
279:over the course of a cycle.
235:detected the variability of
3315:10.1088/0004-637X/785/2/161
3203:10.1088/0004-637X/747/2/145
1153:Clarke, Agnes Mary (1903).
515:, 10–20 days belong to the
4242:
3469:10.1051/0004-6361:20065690
3438:Astronomy and Astrophysics
3342:Astronomy and Astrophysics
2599:10.1051/0004-6361:20040307
2568:Astronomy and Astrophysics
2122:AIP Conference Proceedings
923:Type II Cepheids include:
660:
562:
480:
419:Classical Cepheid variable
416:
29:
4130:
3284:The Astrophysical Journal
3172:The Astrophysical Journal
2970:The Astrophysical Journal
2915:The Astrophysical Journal
2859:The Astrophysical Journal
2063:The Astrophysical Journal
1974:10.1007/s00159-008-0012-y
1883:The Astrophysical Journal
1808:10.1007/s10509-009-0258-5
1368:Astronomische Nachrichten
328:the Universe is expanding
3563:Las Campanas Observatory
3523:10.3847/1538-4365/abd4e3
3228:The Astronomical Journal
3117:The Astronomical Journal
2743:The Astronomical Journal
1161:Adam & Charles Black
1156:Problems in Astrophysics
1110:Goodricke, John (1786).
363:Arthur Stanley Eddington
32:Cepheid (disambiguation)
3773:Solar-like oscillations
3714:Slowly pulsating B-type
3461:2007A&A...461..613S
3354:1981A&A...104...47A
2591:2004A&A...424..927C
2026:2010ARA&A..48..673F
1966:2008A&ARv..15..289T
1829:Rodgers, A. W. (1957).
1800:2010Ap&SS.326..219T
1009:10.1888/0333750888/4130
983:1984S&T....68..519S
231:On September 10, 1784,
3850:Luminous blue variable
3681:Rapidly oscillating Ap
1878:Hubble Space Telescope
1858:10.1093/mnras/117.1.85
1724:Астрономический журнал
1139:10.1098/rstl.1786.0002
1089:10.1098/rstl.1785.0007
1032:Maeder, André (2009).
875:
838:
736:
690:found in electronics.
658:
500:
435:
342:
257:Henrietta Swan Leavitt
228:
150:Henrietta Swan Leavitt
57:
53:Hubble Space Telescope
3383:John Wiley & Sons
1658:Astrophysical Journal
1330:Astrophysical Journal
1293:Astrophysical Journal
1184:Engle, Scott (2015).
876:
846:one finally obtains:
839:
737:
688:relaxation oscillator
656:
565:Fundamental frequency
490:
426:
391:Delta Scuti variables
340:
219:
200:in the constellation
40:
4038:Rotating ellipsoidal
3946:AM Canum Venaticorum
3893:RS Canum Venaticorum
1569:Astronomical Journal
1394:Shapley, H. (1918).
1212:10.5281/zenodo.45252
852:
750:
707:
559:Double-mode Cepheids
314:In 1929, Hubble and
271:. However, in 1914,
4226:Pulsating variables
4075:α Canum Venaticorum
3514:2021ApJS..253...11P
3422:1996AstL...22..326G
3307:2014ApJ...785..161R
3251:2002AJ....124.1695B
3195:2012ApJ...747..145M
3140:1999AJ....117..354D
3101:2010AcA....60..121M
3052:2009MNRAS.396.1287S
2993:2009ApJ...696.1498M
2938:2008ApJ...684..102B
2882:2006ApJ...652.1133M
2843:2001AcA....51..221U
2766:2007AJ....133.1810B
2726:2008AcA....58..153S
2686:2008AcA....58..233S
2647:2008AcA....58..293S
2530:2009MNRAS.397..933M
2487:2010JAVSO..38..100M
2448:2009AcA....59..403M
2388:2008MNRAS.386.2115F
2327:2006MNRAS.370.1979M
2284:2003AcA....53..117K
2245:2008AcA....58..293S
2184:2009MNRAS.398..263M
2130:2009AIPC.1170...23M
2086:2006ApJ...642L..29N
1906:2001ApJ...553...47F
1849:1957MNRAS.117...85R
1758:1996JRASC..90...82T
1708:1917Obs....40..290E
1671:1918ApJ....48..279S
1642:1918CMWCI.153....1S
1582:1958AJ.....63..207B
1537:2002PASP..114..689W
1482:1927ASSB...47...49L
1453:1925Obs....48..139H
1414:1918PASP...30...42S
1381:1913AN....196..201H
1342:1916ApJ....44..273S
1305:1914ApJ....40..448S
1274:1912HarCi.173....1L
1245:1908AnHar..60...87L
1204:2015PhDT........45E
1159:. London, England:
1130:1786RSPT...76...48G
1081:1785RSPT...75..127P
574:Uncertain distances
517:W Virginis subclass
4059:FK Comae Berenices
3855:R Coronae Borealis
3645:Classical cepheids
871:
834:
732:
659:
542:Anomalous Cepheids
501:
436:
413:Classical Cepheids
399:RR Lyrae variables
383:classical Cepheids
343:
229:
133:; a strong direct
58:
4211:Cepheid variables
4152:
4151:
4117:Planetary transit
4093:
4092:
4014:
4007:
3988:
3974:
3956:Luminous red nova
3932:
3931:
3914:Gamma Cassiopeiae
3867:Yellow hypergiant
3863:
3831:
3824:
3786:
3785:
3672:
3652:
3559:Warsaw University
3409:Astronomy Letters
3392:978-0-470-09222-4
2138:10.1063/1.3246452
1876:Results from the
1375:(4692): 201–208.
1170:978-0-403-01478-1
1051:978-3-540-76948-4
970:Sky and Telescope
863:
815:
782:
730:
729:
532:globular clusters
521:RV Tauri subclass
403:horizontal branch
395:instability strip
359:stellar pulsation
357:The mechanics of
316:Milton L. Humason
311:in the Universe.
284:Ejnar Hertzsprung
261:Magellanic Clouds
154:Magellanic Clouds
123:pulsates radially
55:
16:(Redirected from
4233:
4221:Standard candles
4193:
4192:
4191:
4181:
4180:
4169:
4168:
4167:
4160:
4139:
4138:
4028:
4010:
4003:
3984:
3970:
3888:FS Canis Majoris
3857:
3827:
3820:
3795:
3658:
3642:
3625:
3605:
3598:
3591:
3582:
3535:
3534:
3525:
3507:
3487:
3481:
3480:
3454:
3452:astro.ph/0609097
3432:
3426:
3425:
3403:
3397:
3396:
3372:
3366:
3365:
3333:
3327:
3326:
3300:
3277:
3271:
3270:
3244:
3242:astro.ph/0206214
3221:
3215:
3214:
3188:
3166:
3160:
3159:
3133:
3131:astro.ph/9809227
3111:
3105:
3104:
3094:
3078:Acta Astronomica
3072:
3066:
3065:
3063:
3045:
3036:(3): 1287–1296.
3019:
3013:
3012:
2986:
2977:(2): 1498–1501.
2964:
2958:
2957:
2931:
2908:
2902:
2901:
2875:
2873:astro.ph/0608211
2866:(2): 1133–1149.
2853:
2847:
2846:
2836:
2834:astro.ph/0109446
2820:Acta Astronomica
2813:
2807:
2806:
2804:
2802:astro-ph/9909346
2792:
2786:
2785:
2759:
2757:astro.ph/0612465
2736:
2730:
2729:
2719:
2703:Acta Astronomica
2696:
2690:
2689:
2679:
2663:Acta Astronomica
2657:
2651:
2650:
2640:
2624:Acta Astronomica
2617:
2611:
2610:
2584:
2582:astro.ph/0405395
2558:
2552:
2551:
2541:
2523:
2497:
2491:
2490:
2480:
2458:
2452:
2451:
2441:
2425:Acta Astronomica
2419:
2410:
2409:
2399:
2381:
2372:(4): 2115–2134.
2355:
2349:
2348:
2338:
2320:
2318:astro.ph/0606609
2311:(4): 1979–1990.
2294:
2288:
2287:
2277:
2275:astro.ph/0306567
2261:Acta Astronomica
2255:
2249:
2248:
2238:
2222:Acta Astronomica
2215:
2206:
2205:
2195:
2177:
2151:
2142:
2141:
2117:
2106:
2105:
2079:
2077:astro.ph/0603643
2057:
2046:
2045:
2019:
1997:
1986:
1985:
1959:
1937:
1926:
1925:
1899:
1897:astro.ph/0012376
1872:
1863:
1862:
1860:
1826:
1820:
1819:
1793:
1771:
1762:
1761:
1739:
1733:
1732:
1718:
1712:
1711:
1689:
1683:
1682:
1652:
1646:
1645:
1623:
1617:
1616:
1615:on Dec 10, 2007.
1611:. Archived from
1600:
1594:
1593:
1563:
1557:
1556:
1531:(797): 689–699.
1518:
1507:
1506:
1504:
1502:
1492:
1486:
1485:
1463:
1457:
1456:
1434:
1428:
1427:
1425:
1391:
1385:
1384:
1362:
1356:
1355:
1353:
1325:
1319:
1318:
1316:
1284:
1278:
1277:
1255:
1249:
1248:
1222:
1216:
1215:
1197:
1181:
1175:
1174:
1150:
1144:
1143:
1141:
1107:
1101:
1100:
1062:
1056:
1055:
1039:
1029:
1023:
1022:
996:
987:
986:
964:
880:
878:
877:
872:
864:
859:
843:
841:
840:
835:
827:
816:
814:
813:
804:
796:
794:
783:
781:
780:
768:
766:
741:
739:
738:
733:
731:
722:
721:
582:, the impact of
477:Type II Cepheids
387:type II Cepheids
373:for the engine.
332:Georges Lemaître
297:Andromeda Galaxy
226:type II Cepheids
204:, identified by
196:originates from
143:pulsation period
116:
115:
112:
111:
108:
105:
102:
99:
94:
93:
90:
87:
84:
81:
78:
75:
72:
62:Cepheid variable
51:
21:
4241:
4240:
4236:
4235:
4234:
4232:
4231:
4230:
4201:
4200:
4199:
4189:
4187:
4175:
4165:
4163:
4155:
4153:
4148:
4141:Star portal
4133:
4126:
4122:W Ursae Majoris
4089:
4068:Magnetic fields
4063:
4042:
4019:
3928:
3897:
3883:Double periodic
3876:Eruptive binary
3871:
3842:
3836:
3782:
3756:
3728:
3696:
3695:Blue-white with
3690:
3632:
3614:
3609:
3544:
3539:
3538:
3489:
3488:
3484:
3434:
3433:
3429:
3405:
3404:
3400:
3393:
3385:. p. 180.
3374:
3373:
3369:
3335:
3334:
3330:
3279:
3278:
3274:
3223:
3222:
3218:
3168:
3167:
3163:
3113:
3112:
3108:
3074:
3073:
3069:
3021:
3020:
3016:
2966:
2965:
2961:
2910:
2909:
2905:
2855:
2854:
2850:
2815:
2814:
2810:
2794:
2793:
2789:
2738:
2737:
2733:
2698:
2697:
2693:
2659:
2658:
2654:
2619:
2618:
2614:
2560:
2559:
2555:
2499:
2498:
2494:
2460:
2459:
2455:
2421:
2420:
2413:
2357:
2356:
2352:
2296:
2295:
2291:
2257:
2256:
2252:
2217:
2216:
2209:
2153:
2152:
2145:
2119:
2118:
2109:
2059:
2058:
2049:
1999:
1998:
1989:
1939:
1938:
1929:
1874:
1873:
1866:
1828:
1827:
1823:
1773:
1772:
1765:
1741:
1740:
1736:
1720:
1719:
1715:
1695:The Observatory
1691:
1690:
1686:
1654:
1653:
1649:
1625:
1624:
1620:
1602:
1601:
1597:
1565:
1564:
1560:
1520:
1519:
1510:
1500:
1498:
1494:
1493:
1489:
1465:
1464:
1460:
1440:The Observatory
1436:
1435:
1431:
1393:
1392:
1388:
1364:
1363:
1359:
1327:
1326:
1322:
1286:
1285:
1281:
1257:
1256:
1252:
1224:
1223:
1219:
1183:
1182:
1178:
1171:
1163:. p. 319.
1152:
1151:
1147:
1109:
1108:
1104:
1064:
1063:
1059:
1052:
1031:
1030:
1026:
1019:
998:
997:
990:
966:
965:
958:
953:
893:
850:
849:
820:
805:
797:
787:
772:
759:
748:
747:
705:
704:
699:surface gravity
665:
663:Kappa–mechanism
651:
649:Pulsation model
640:
595:Hubble constant
576:
567:
561:
551:formed through
549:blue stragglers
544:
528:Galactic Center
513:BL Her subclass
491:Light curve of
485:
483:Type II Cepheid
479:
463:Hubble constant
421:
415:
407:kappa mechanism
379:
265:radial velocity
214:
190:
158:true luminosity
117:) is a type of
96:
69:
65:
49:
35:
28:
23:
22:
15:
12:
11:
5:
4239:
4237:
4229:
4228:
4223:
4218:
4213:
4203:
4202:
4198:
4197:
4185:
4173:
4150:
4149:
4131:
4128:
4127:
4125:
4124:
4119:
4114:
4109:
4103:
4101:
4095:
4094:
4091:
4090:
4088:
4087:
4082:
4077:
4071:
4069:
4065:
4064:
4062:
4061:
4056:
4050:
4048:
4044:
4043:
4041:
4040:
4034:
4032:
4025:
4021:
4020:
4018:
4017:
4016:
4015:
4008:
4005:Symbiotic nova
3996:
3991:
3990:
3989:
3977:
3976:
3975:
3963:
3958:
3953:
3948:
3942:
3940:
3934:
3933:
3930:
3929:
3927:
3926:
3921:
3919:Lambda Eridani
3916:
3911:
3905:
3903:
3899:
3898:
3896:
3895:
3890:
3885:
3879:
3877:
3873:
3872:
3870:
3869:
3864:
3852:
3846:
3844:
3838:
3837:
3835:
3834:
3833:
3832:
3825:
3813:
3807:
3805:
3792:
3788:
3787:
3784:
3783:
3781:
3780:
3775:
3770:
3764:
3762:
3758:
3757:
3755:
3754:
3752:Slow irregular
3749:
3744:
3738:
3736:
3730:
3729:
3727:
3726:
3721:
3716:
3711:
3706:
3700:
3698:
3692:
3691:
3689:
3688:
3683:
3678:
3673:
3653:
3636:
3634:
3622:
3616:
3615:
3612:Variable stars
3610:
3608:
3607:
3600:
3593:
3585:
3579:
3578:
3573:
3555:
3550:
3543:
3542:External links
3540:
3537:
3536:
3482:
3445:(2): 613–618.
3427:
3398:
3391:
3367:
3328:
3272:
3259:10.1086/342014
3216:
3161:
3148:10.1086/300682
3124:(1): 354–399.
3106:
3067:
3014:
2959:
2946:10.1086/589965
2922:(1): 102–117.
2903:
2890:10.1086/508530
2848:
2808:
2787:
2774:10.1086/511980
2731:
2691:
2652:
2612:
2575:(3): 927–934.
2553:
2514:(2): 933–942.
2492:
2471:(1): 100–112.
2453:
2411:
2350:
2289:
2250:
2207:
2168:(1): 263–270.
2143:
2107:
2094:10.1086/504478
2070:(1): L29–L32.
2047:
1987:
1950:(4): 289–331.
1927:
1914:10.1086/320638
1864:
1821:
1784:(2): 219–231.
1763:
1734:
1713:
1684:
1679:10.1086/142435
1647:
1618:
1595:
1590:10.1086/107726
1558:
1545:10.1086/341698
1508:
1487:
1458:
1429:
1423:10.1086/122686
1386:
1357:
1351:10.1086/142295
1320:
1314:10.1086/142137
1279:
1250:
1217:
1176:
1169:
1145:
1102:
1057:
1050:
1024:
1017:
988:
955:
954:
952:
949:
948:
947:
936:
921:
902:Zeta Geminorum
892:
889:
870:
867:
862:
857:
833:
830:
826:
823:
819:
812:
808:
803:
800:
793:
790:
786:
779:
775:
771:
765:
762:
758:
755:
728:
725:
718:
715:
712:
650:
647:
638:
575:
572:
560:
557:
543:
540:
481:Main article:
478:
475:
448:spectral class
444:variable stars
417:Main article:
414:
411:
378:
375:
367:S. A. Zhevakin
277:spectral types
273:Harlow Shapley
245:John Goodricke
213:
210:
206:John Goodricke
189:
186:
181:doubly ionized
26:
24:
14:
13:
10:
9:
6:
4:
3:
2:
4238:
4227:
4224:
4222:
4219:
4217:
4214:
4212:
4209:
4208:
4206:
4196:
4186:
4184:
4179:
4174:
4172:
4162:
4158:
4147:
4143:
4142:
4137:
4129:
4123:
4120:
4118:
4115:
4113:
4110:
4108:
4105:
4104:
4102:
4100:
4096:
4086:
4083:
4081:
4078:
4076:
4073:
4072:
4070:
4066:
4060:
4057:
4055:
4052:
4051:
4049:
4047:Stellar spots
4045:
4039:
4036:
4035:
4033:
4031:Non-spherical
4029:
4026:
4022:
4013:
4009:
4006:
4002:
4001:
4000:
3997:
3995:
3992:
3987:
3983:
3982:
3981:
3978:
3973:
3969:
3968:
3967:
3964:
3962:
3959:
3957:
3954:
3952:
3949:
3947:
3944:
3943:
3941:
3939:
3935:
3925:
3922:
3920:
3917:
3915:
3912:
3910:
3907:
3906:
3904:
3900:
3894:
3891:
3889:
3886:
3884:
3881:
3880:
3878:
3874:
3868:
3865:
3861:
3856:
3853:
3851:
3848:
3847:
3845:
3839:
3830:
3826:
3823:
3819:
3818:
3817:
3814:
3812:
3809:
3808:
3806:
3804:
3800:
3796:
3793:
3789:
3779:
3776:
3774:
3771:
3769:
3768:Gamma Doradus
3766:
3765:
3763:
3759:
3753:
3750:
3748:
3745:
3743:
3740:
3739:
3737:
3735:
3731:
3725:
3722:
3720:
3719:PV Telescopii
3717:
3715:
3712:
3710:
3707:
3705:
3702:
3701:
3699:
3697:early spectra
3693:
3687:
3684:
3682:
3679:
3677:
3674:
3670:
3666:
3662:
3657:
3654:
3650:
3646:
3641:
3638:
3637:
3635:
3630:
3626:
3623:
3621:
3617:
3613:
3606:
3601:
3599:
3594:
3592:
3587:
3586:
3583:
3577:
3574:
3572:
3568:
3564:
3560:
3556:
3554:
3551:
3549:
3546:
3545:
3541:
3533:
3529:
3524:
3519:
3515:
3511:
3506:
3501:
3497:
3493:
3486:
3483:
3478:
3474:
3470:
3466:
3462:
3458:
3453:
3448:
3444:
3440:
3439:
3431:
3428:
3423:
3419:
3415:
3411:
3410:
3402:
3399:
3394:
3388:
3384:
3380:
3379:
3371:
3368:
3363:
3359:
3355:
3351:
3347:
3343:
3339:
3332:
3329:
3324:
3320:
3316:
3312:
3308:
3304:
3299:
3294:
3290:
3286:
3285:
3276:
3273:
3268:
3264:
3260:
3256:
3252:
3248:
3243:
3238:
3234:
3230:
3229:
3220:
3217:
3212:
3208:
3204:
3200:
3196:
3192:
3187:
3182:
3178:
3174:
3173:
3165:
3162:
3157:
3153:
3149:
3145:
3141:
3137:
3132:
3127:
3123:
3119:
3118:
3110:
3107:
3102:
3098:
3093:
3088:
3084:
3080:
3079:
3071:
3068:
3062:
3057:
3053:
3049:
3044:
3039:
3035:
3031:
3030:
3025:
3018:
3015:
3010:
3006:
3002:
2998:
2994:
2990:
2985:
2980:
2976:
2972:
2971:
2963:
2960:
2955:
2951:
2947:
2943:
2939:
2935:
2930:
2925:
2921:
2917:
2916:
2907:
2904:
2899:
2895:
2891:
2887:
2883:
2879:
2874:
2869:
2865:
2861:
2860:
2852:
2849:
2844:
2840:
2835:
2830:
2826:
2822:
2821:
2812:
2809:
2803:
2798:
2791:
2788:
2783:
2779:
2775:
2771:
2767:
2763:
2758:
2753:
2749:
2745:
2744:
2735:
2732:
2727:
2723:
2718:
2713:
2709:
2705:
2704:
2695:
2692:
2687:
2683:
2678:
2673:
2669:
2665:
2664:
2656:
2653:
2648:
2644:
2639:
2634:
2630:
2626:
2625:
2616:
2613:
2608:
2604:
2600:
2596:
2592:
2588:
2583:
2578:
2574:
2570:
2569:
2564:
2557:
2554:
2549:
2545:
2540:
2535:
2531:
2527:
2522:
2517:
2513:
2509:
2508:
2503:
2496:
2493:
2488:
2484:
2479:
2474:
2470:
2466:
2465:
2457:
2454:
2449:
2445:
2440:
2435:
2431:
2427:
2426:
2418:
2416:
2412:
2407:
2403:
2398:
2393:
2389:
2385:
2380:
2375:
2371:
2367:
2366:
2361:
2354:
2351:
2346:
2342:
2337:
2332:
2328:
2324:
2319:
2314:
2310:
2306:
2305:
2300:
2293:
2290:
2285:
2281:
2276:
2271:
2267:
2263:
2262:
2254:
2251:
2246:
2242:
2237:
2232:
2228:
2224:
2223:
2214:
2212:
2208:
2203:
2199:
2194:
2189:
2185:
2181:
2176:
2171:
2167:
2163:
2162:
2157:
2150:
2148:
2144:
2139:
2135:
2131:
2127:
2123:
2116:
2114:
2112:
2108:
2103:
2099:
2095:
2091:
2087:
2083:
2078:
2073:
2069:
2065:
2064:
2056:
2054:
2052:
2048:
2043:
2039:
2035:
2031:
2027:
2023:
2018:
2013:
2009:
2005:
2004:
1996:
1994:
1992:
1988:
1983:
1979:
1975:
1971:
1967:
1963:
1958:
1953:
1949:
1945:
1944:
1936:
1934:
1932:
1928:
1923:
1919:
1915:
1911:
1907:
1903:
1898:
1893:
1889:
1885:
1884:
1879:
1871:
1869:
1865:
1859:
1854:
1850:
1846:
1842:
1838:
1837:
1832:
1825:
1822:
1817:
1813:
1809:
1805:
1801:
1797:
1792:
1787:
1783:
1779:
1778:
1770:
1768:
1764:
1759:
1755:
1751:
1747:
1746:
1738:
1735:
1730:
1726:
1725:
1717:
1714:
1709:
1705:
1701:
1697:
1696:
1688:
1685:
1680:
1676:
1672:
1668:
1664:
1660:
1659:
1651:
1648:
1643:
1639:
1635:
1631:
1630:
1622:
1619:
1614:
1610:
1606:
1603:Allen, Nick.
1599:
1596:
1591:
1587:
1583:
1579:
1575:
1571:
1570:
1562:
1559:
1554:
1550:
1546:
1542:
1538:
1534:
1530:
1526:
1525:
1517:
1515:
1513:
1509:
1497:
1491:
1488:
1483:
1479:
1475:
1471:
1470:
1462:
1459:
1454:
1450:
1446:
1442:
1441:
1433:
1430:
1424:
1419:
1415:
1411:
1407:
1403:
1402:
1397:
1390:
1387:
1382:
1378:
1374:
1371:(in German).
1370:
1369:
1361:
1358:
1352:
1347:
1343:
1339:
1335:
1331:
1324:
1321:
1315:
1310:
1306:
1302:
1298:
1294:
1290:
1283:
1280:
1275:
1271:
1267:
1263:
1262:
1254:
1251:
1246:
1242:
1239:(4): 87–108.
1238:
1234:
1233:
1228:
1221:
1218:
1213:
1209:
1205:
1201:
1196:
1191:
1187:
1180:
1177:
1172:
1166:
1162:
1158:
1157:
1149:
1146:
1140:
1135:
1131:
1127:
1123:
1119:
1118:
1113:
1106:
1103:
1098:
1094:
1090:
1086:
1082:
1078:
1074:
1070:
1069:
1061:
1058:
1053:
1047:
1043:
1038:
1037:
1028:
1025:
1020:
1018:0-333-75088-8
1014:
1010:
1006:
1002:
995:
993:
989:
984:
980:
976:
972:
971:
963:
961:
957:
950:
945:
941:
937:
934:
930:
929:Kappa Pavonis
926:
922:
919:
916:, as well as
915:
911:
907:
903:
899:
895:
894:
890:
888:
886:
881:
868:
865:
860:
855:
847:
844:
831:
828:
824:
821:
817:
810:
806:
801:
798:
791:
788:
784:
777:
773:
769:
763:
760:
756:
753:
745:
742:
726:
723:
716:
713:
710:
702:
700:
696:
695:August Ritter
691:
689:
685:
680:
676:
672:
670:
664:
655:
648:
646:
644:
636:
632:
627:
623:
619:
615:
611:
607:
602:
600:
596:
591:
589:
585:
581:
573:
571:
566:
558:
556:
554:
553:mass transfer
550:
541:
539:
537:
533:
529:
524:
522:
518:
514:
510:
506:
505:population II
498:
494:
489:
484:
476:
474:
472:
467:
464:
460:
455:
453:
449:
445:
442:
433:
429:
425:
420:
412:
410:
408:
404:
400:
396:
392:
388:
384:
376:
374:
372:
368:
364:
360:
355:
353:
348:
339:
335:
333:
329:
325:
324:Vesto Slipher
321:
317:
312:
310:
306:
302:
298:
294:
290:
285:
280:
278:
274:
270:
269:binary system
266:
262:
258:
253:
251:
246:
242:
238:
234:
233:Edward Pigott
227:
223:
218:
211:
209:
207:
203:
199:
195:
187:
185:
182:
178:
174:
169:
167:
163:
159:
155:
151:
146:
144:
140:
136:
132:
128:
124:
120:
119:variable star
114:
63:
54:
47:
43:
39:
33:
19:
4132:
4012:Z Andromedae
3994:SW Sextantis
3972:Intermediate
3811:Herbig Ae/Be
3686:SX Phoenicis
3633:cepheid-like
3628:
3565:: OGLE-III (
3495:
3491:
3485:
3442:
3436:
3430:
3413:
3407:
3401:
3377:
3370:
3348:(1): 47–56.
3345:
3341:
3331:
3288:
3282:
3275:
3232:
3226:
3219:
3176:
3170:
3164:
3121:
3115:
3109:
3082:
3076:
3070:
3033:
3027:
3017:
2974:
2968:
2962:
2919:
2913:
2906:
2863:
2857:
2851:
2824:
2818:
2811:
2790:
2747:
2741:
2740:Relations".
2734:
2707:
2701:
2694:
2667:
2661:
2655:
2628:
2622:
2615:
2572:
2566:
2565:Cepheids?".
2562:
2556:
2511:
2505:
2495:
2468:
2462:
2456:
2429:
2423:
2369:
2363:
2353:
2308:
2302:
2292:
2265:
2259:
2253:
2226:
2220:
2165:
2159:
2121:
2067:
2061:
2007:
2001:
1947:
1941:
1890:(1): 47–72.
1887:
1881:
1877:
1840:
1834:
1824:
1781:
1775:
1749:
1743:
1737:
1728:
1722:
1716:
1699:
1693:
1687:
1662:
1656:
1650:
1633:
1627:
1621:
1613:the original
1608:
1598:
1573:
1567:
1561:
1528:
1522:
1499:. Retrieved
1490:
1473:
1467:
1461:
1444:
1438:
1432:
1405:
1399:
1389:
1372:
1366:
1360:
1333:
1329:
1323:
1296:
1292:
1282:
1265:
1259:
1253:
1236:
1230:
1220:
1185:
1179:
1155:
1148:
1121:
1115:
1105:
1072:
1066:
1060:
1035:
1027:
1000:
974:
968:
918:Delta Cephei
906:Beta Doradus
884:
882:
848:
845:
746:
743:
703:
692:
673:
666:
610:star cluster
603:
592:
577:
568:
545:
525:
502:
468:
456:
441:Population I
437:
432:Delta Cephei
380:
371:likely valve
356:
347:Walter Baade
344:
320:Hubble's Law
313:
305:Great Debate
293:Edwin Hubble
281:
254:
241:Delta Cephei
230:
198:Delta Cephei
193:
191:
170:
157:
147:
135:relationship
61:
59:
4195:Outer space
4054:BY Draconis
3938:Cataclysmic
3843:supergiants
3778:White dwarf
3747:Semiregular
3734:Long-period
3709:Beta Cephei
3704:Alpha Cygni
3661:BL Herculis
3649:Delta Scuti
3235:(3): 1695.
2750:(4): 1810.
2010:: 673–710.
1665:: 279–294.
1408:(173): 42.
1075:: 127–136.
933:BL Herculis
898:Eta Aquilae
669:κ-mechanism
584:metallicity
459:Local Group
428:Light curve
250:ζ Geminorum
237:Eta Aquilae
173:κ–mechanism
4216:Astrometry
4205:Categories
4112:Beta Lyrae
4085:SX Arietis
3951:Dwarf nova
3924:Wolf–Rayet
3841:Giants and
3822:FU Orionis
3665:W Virginis
3557:Survey of
3505:2012.09709
3416:(3): 326.
3291:(2): 161.
3179:(2): 145.
3085:(2): 121.
2432:(4): 403.
1731:: 161–179.
1501:29 October
1195:1504.02713
1188:(Thesis).
951:References
925:W Virginis
910:RT Aurigae
684:hysterisis
661:See also:
643:resolution
606:calibrator
588:extinction
563:See also:
471:sinusoidal
352:magnitudes
139:luminosity
4171:Astronomy
4099:Eclipsing
3999:Symbiotic
3986:Hypernova
3980:Supernova
3860:DY Persei
3799:Protostar
3620:Pulsating
3532:229297708
3498:(1): 11,
3362:0004-6361
3298:1401.0484
3211:118672744
3186:1201.0993
3092:1006.2458
3043:0903.4088
2984:0902.3747
2929:0805.1592
2717:0807.4182
2677:0809.1986
2638:0811.3636
2563:Anomalous
2521:0904.4701
2478:0912.2928
2439:0909.0181
2379:0803.0466
2236:0811.3636
2175:0903.4206
2017:1004.1856
1957:0806.3018
1922:119097691
1843:: 85–94.
1816:119264970
1791:0912.4864
1553:122225966
1124:: 48–61.
1097:186212958
944:BL Boötis
861:ρ
832:ρ
693:In 1879,
618:Hipparcos
599:RS Puppis
580:passbands
493:κ Pavonis
452:I Carinae
289:Milky Way
282:In 1913,
192:The term
188:Etymology
46:Milky Way
42:RS Puppis
4024:Rotating
3791:Eruptive
3676:RR Lyrae
3669:RV Tauri
3629:Cepheids
3477:18245078
3323:55928992
3267:42655824
3156:16098861
3009:16325249
2898:15728812
2782:16384267
2607:45306570
2548:13912466
2406:14459638
2345:25991504
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