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Type of variable star
Classical Cepheids are a type of Cepheid variable star. They are young, population I variable stars that exhibit regular radial pulsations with periods
Classical_Cepheid_variable
Type of variable star that pulsates radially
A Cepheid variable (/ˈsɛfi.ɪd, ˈsiːfi-/) is a type of variable star that pulsates radially, varying in both diameter and temperature. It changes in brightness
Cepheid_variable
Astronomical principle
pulsating variable stars with their pulsation period. The best-known relation is the direct proportionality law holding for Classical Cepheid variables, sometimes
Period-luminosity_relation
Northern pole-star; brightest star in Ursa Minor
population I classical Cepheid variable, although it was once thought to be a type II Cepheid due to its high galactic latitude. Cepheids constitute an
Polaris
Variable star in the constellation Centaurus
V Centauri (V Cen) is a Classical Cepheid variable, a type of variable star, in the constellation Centaurus. It is approximately 2,350 light-years (720
V_Centauri
Star whose brightness fluctuates, as seen from Earth
class of variables is named after Beta Cephei. Classical Cepheid variables Type I cepheids, also called Classical Cepheids or Delta Cephei variables, are
Variable_star
Variable star in the constellation Dorado
brightest star in the southern constellation of Dorado. It is a Classical Cepheid variable, with an apparent magnitude that varies between 3.46 and 4.08
Beta_Doradus
Cepheid Variable in constellation of Monoceros
T Monocerotis (T Mon) is a classical Cepheid variable star in the constellation of Monoceros, visually located 2° northwest of Epsilon Monocerotis. Along
T_Monocerotis
Variable star in the constellation Cygnus
naked eye of an observer located far from city lights. It is a classical Cepheid variable star, ranging in brightness from magnitude 5.77 to 5.96 over a
V1334_Cygni
Star in the constellation Vulpecula
an RV Tauri variable, a semiregular variable star, or a Cepheid variable. S Vulpeculae is now confirmed as a classical Cepheid variable with one of the
S_Vulpeculae
Subclass of pulsating star
A Delta Scuti variable (sometimes termed dwarf cepheid when the V-band amplitude is larger than 0.3 mag.) is a class of pulsating star, comprising several
Delta_Scuti_variable
Binary star system in the constellation Cepheus
the prototype of the Cepheid variable stars that undergo periodic changes in luminosity. Delta Cephei was discovered to be variable by John Goodricke during
Delta_Cephei
Star in the constellation Lyra
V473 Lyrae is a variable star in the constellation Lyra. It is an unusual Classical Cepheid variable with a visual range of 5.99 to 6.35. V473 Lyrae is
V473_Lyrae
Variable star in the Large Magellanic Cloud
their understanding of classical Cepheid variable stars. Studies of this system have allowed astronomers to measure the Cepheid mass with unprecedented
OGLE-LMC-CEP0227
Variable star in the constellation Puppis
Pup) is a Cepheid variable star around 6,000 ly away in the constellation of Puppis. It is one of the biggest and brightest known Cepheids in the Milky
RS_Puppis
Star in the constellation Carina
Y Carinae (Y Car) is a Classical Cepheid variable, a type of variable star, in the constellation Carina. Its apparent magnitude varies from 7.53 to 8.48
Y_Carinae
Star in the constellation Gemini
— in its south, on the left 'leg' of the twin Pollux. It is a classical Cepheid variable star, of which over 800 have been found in our galaxy. As such
Zeta_Geminorum
Multiple star in the constellation Aquila
approximately 272 parsecs (890 light-years). The primary component is a Classical Cepheid variable. Eta Aquilae is a Bayer designation that is Latinized from η Aquilae
Eta_Aquilae
Index of articles associated with the same name
Carinae are distinct and refer to two different stars: W Carinae, a classical Cepheid variable in the constellation Vela that is now called V Velorum w Carinae
W_Carinae
Variable star in the constellation Crux
X Crucis is a classical Cepheid variable star in the southern constellation of Crux. X Crucis is a pulsating variable star with am extremely regular amplitude
X_Crucis
Star in the constellation Carina
a Classical Cepheid variable, a type of variable star, in the constellation Carina. Its apparent magnitude is 6.86. U Car is a δ Cepheid variable with
HD_95109
Star in the constellation Carina
million years as a main sequence star. l Carinae is classified as a Cepheid variable star and its brightness varies over an amplitude range of 0.725 in
HD_84810
Star in the constellation Norma
supergiant variable star in the constellation Norma. It is the brightest member of the open cluster NGC 6087. S Normae is a Classical Cepheid variable with
S_Normae
American astronomer (1889–1953)
Milky Way. He used the strong direct relationship between a classical Cepheid variable's luminosity and pulsation period (discovered in 1908 by Henrietta
Edwin_Hubble
Star that has a supergiant luminosity class, with a spectral type of F or G
including W Virginis variables, BL Herculis variables and RV Tauri variables. The Classical Cepheids are more luminous than the type II Cepheids with the same
Yellow_supergiant
Star in the constellation Leo
gas and dust. Epsilon Leonis exhibits the characteristics of a Cepheid-like variable, changing by an amplitude of 0.3 magnitude every few days. It has
Epsilon_Leonis
Variable star in the constellation Crux
F6Ib-II and G1Ib-II. S Crucis is a pulsating variable star of the δ Cephei type, a Classical Cepheid variable. Its mean radius is 37.9 R☉ and that radius
S_Crucis
Variable star in the constellation Cygnus
identified as a member of the benchmark class of stars termed Classical Cepheid variables that satisfy a simple period-luminosity relation. In 1954, R
X_Cygni
Type of variable stars
Type II Cepheids are variable stars which pulsate with periods typically between 1 and 50 days. They are population II stars: old, typically metal-poor
Type_II_Cepheid
Star in the constellation Cassiopeia
variable stars pulsate in a regular manner with periods related to their luminosity. It is slightly hotter and more luminous than classical Cepheid variable
HD_18391
Variable star in the constellation Musca
star with a baseline stellar classification of F7 Ib. It is a Classical Cepheid variable ranging from apparent magnitude 5.93 to 6.73 over 7.51 days, while
R_Muscae
Star in the constellation Sagittarius
multiple star system star in the constellation Sagittarius, and a Cepheid variable star. W Sagittarii is an optical line-of-sight companion nearly a degree
W_Sagittarii
Type of variable star
and BL Herculis variables, the type II Cepheids. Classical Cepheid variables are higher mass population I stars. RR Lyrae variables are much more common
RR_Lyrae_variable
Variable star in the constellation Antlia
T Antliae (also abbreviated T Ant) is a Classical Cepheid variable star that is between 10 and 12,000 light-years away from the Sun in the constellation
T_Antliae
International collaboration to improve calibration of the extragalactic distance scale
300 and NGC 7793 in the Sculptor Group. The dynamical mass of a classical Cepheid variable star in an eclipsing binary system RR-Lyrae-type pulsations from
Araucaria_Project
Star in the constellation Sagittarius
U Sagittarii is a variable star in the southern constellation of Sagittarius, abbreviated U Sgr. It is a classical Cepheid variable that ranges in brightness
U_Sagittarii
American astronomer (1868–1921)
to discover the relation between the luminosity and the period of Cepheid variables. Leavitt's discovery provided astronomers with the first standard
Henrietta_Swan_Leavitt
Variable star in the constellation Vulpecula
It is a classical Cepheid variable and its apparent magnitude ranges from 6.73 to 7.54 over a precise cycle of 7.99 days. Its variable nature was discovered
U_Vulpeculae
Variable star in the constellation Sagitta
Sagittae, also known by the Flamsteed designation of 10 Sagittae, a Classical Cepheid variable in the constellation Sagitta that varies from magnitude 5.24 to
S_Sagittae
Yellow-white hued star in the constellation Vela
from its photosphere at an effective temperature of 6,102 K. A classical Cepheid variable, its apparent magnitude ranges from 5.50 to 5.89 over 4.227171
AH_Velorum
Star and possible star system in the constellation Aquila
FF Aquilae is a classical Cepheid variable star located in the constellation Aquila, close to the border with Hercules. It ranges from apparent magnitude
FF_Aquilae
Binary star system in the constellation Circinus
that it is a variable star, in 1964, but could not classify it initially. By 1966 he had classified it as a classical Cepheid variable. The combined
AX_Circini
Star system in the Crux constellation
between spectral types F5Ib and G0p. It is a small amplitude classical Cepheid variable with an apparent magnitude ranges from 5.34 down to 5.58 over
BG_Crucis
Type of variable stars
W Virginis variables are a subclass of Type II Cepheids which exhibit pulsation periods between 10–20 days, and are of spectral class F6 – K2. They were
W_Virginis_variable
Binary star in the constellation Hercules
to be a type II Cepheid and thus is instead an anomalous Cepheid, an object located between classical Cepheids and type II Cepheids in the Hertzsprung-Russell
TYC_1031-1262-1
Star in the constellation Centaurus
corresponds to Cepheid fundamental mode radial pulsation. Without the other stellar pulsation modes it would be considered a Classical Cepheid variable. Other
V810_Centauri
Star in the constellation Auriga
under good observing conditions. RT Aurigae is an F to G type Classical Cepheid variable which varies from magnitude +5.00 to +5.82 with a period of 3
RT_Aurigae
Variable star in Taurus
confirmed to be a classical Cepheid by W. P. Gieren in 1985. In the General Catalogue of Variable Stars, SZ Tau is classified as a Delta Cepheid of type DCEPS
SZ_Tauri
Variable star system in the constellation Cygnus
abbreviated SU Cyg. The primary component of the system is a classical Cepheid variable with a period of 3.84559 days. The changing luminosity of this
SU_Cygni
Variable star in the constellation Triangulum Australe
published that discovery in his 1879 work Uranometria Argentina. A Classical Cepheid variable, its apparent magnitude ranges from 5.95 to 6.81 over 6.32344
S_Trianguli_Australis
Star in the constellation Aquila
TT Aquilae (TT Aql) is a Classical Cepheid (δ Cep) variable star in the constellation Aquila. The visual apparent magnitude of TT Aql ranges from 6.52
TT_Aquilae
Open star cluster in the constellation Cassiopeia
astrometric solutions, evolutionary ages, and radial velocities. Four classical Cepheid variables (CE Cas A, CE Cas B, CF Cas, and CG Cas) were identified as possible
NGC_7790
Variable star in the constellation Vulpecula
determined from its annual parallax shift of 1.67 mas. A well-studied Classical Cepheid variable and one of the brightest known, the apparent magnitude of T Vulpeculae
T_Vulpeculae
Globular cluster in the constellation Dorado
has 65 variable stars that have been identified. Among them are 53 RR Lyrae variables, along with 3 classical Cepheids, a single Type II Cepheid, 1 anomalous
NGC_1786
Succession of methods by which astronomers determine the distances to celestial objects
of classical Cepheid variable stars. The following relation can be used to calculate the distance to Galactic and extragalactic classical Cepheids:
Cosmic_distance_ladder
Variable binary star system in the constellation Aquila
its variable star designation, U Aquilae, in Annie Jump Cannon's 1907 Second Catalogue of Variable Stars. U Aquilae Aa is a classical Cepheid variable star
U_Aquilae
time, regularly or irregularly pulsating over several months or years as variable stars. This makes adopted luminosities poorly known and may significantly
List_of_largest_stars
Star in the constellation Musca
S Muscae is a classical (δ) Cepheid variable star in the constellation Musca about 2,800 light years away. S Muscae is a yellow supergiant ranging between
S_Muscae
Variable star in the constellation Triangulum Australe
discovered that the star's brightness varies, in 1871. This is a Classical Cepheid variable with an apparent magnitude that ranges from 6.33 to 6.90 over
R_Trianguli_Australis
Star in the constellation Vulpecula
SV Vulpeculae is a classical Cepheid (δ Cepheid) variable star in the constellation Vulpecula. It is a supergiant at a distance of 8,700 light years. It
SV_Vulpeculae
Spectroscopic binary star system in the constellation Scorpius
constellation Scorpius, 3,000 light years away. The primary is a Classical Cepheid (δ Cephei) variable and its visual magnitude varies from 6.4 to 6.9. V636 Scorpii
V636_Scorpii
Type of star that is massive and luminous
have supergiant luminosity classes, for example α Herculis. Classical Cepheid variables typically have supergiant luminosity classes, although only the
Supergiant
Variable star and possible binary star system in the constellation Sagittarius
the star is a variable star. This is an F-type bright giant with a stellar classification of F7II. It is a Classical Cepheid variable that ranges in
X_Sagittarii
Constellation in the southern celestial hemisphere
have been found to have planets. The constellation also contains two cepheid variables visible to the naked eye. Theta Muscae is a triple star system, the
Musca
Star in the constellation Circinus
this star was discovered by D. W. Kurtz in 1979. A small-amplitude Cepheid variable, its apparent magnitude ranges from 7.37 to 7.71 over 2.39810 days
BP_Circini
Variable star in the constellation Crux
closer with a radial velocity of −13.5 km/s. This is a Classical Cepheid, or Delta Cephei variable, that ranges in brightness from visual magnitude 6.40
R_Crucis
Star in the constellation Boötes
class of anomalous Cepheids which is intermediate in the H-R diagram between the type I classical Cepheids and the type II Cepheids. It varies from magnitude
BL_Boötis
(2014-09-25). "The Secret Lives of Cepheids: Evolutionary Changes and Pulsation-Induced Shock Heating in the Prototype Classical Cepheid {\delta} Cep". The Astrophysical
List_of_nearest_supergiants
Fluctuations in stellar radius
the Doppler effect. Many intrinsic variable stars that pulsate with large amplitudes, such as the classical Cepheids, RR Lyrae stars and large-amplitude
Stellar_pulsation
Variable star in the constellation Crux
T Crucis is a star in the constellation Crux. A Cepheid variable, its apparent magnitude ranges from 6.32 to 6.83 over 6.73331 days. It is a yellow-white
T_Crucis
Dark satellite dwarf galaxy of the Milky Way Galaxy
galaxy was presented in 2015, based on the claimed discovery of four Cepheid variable stars by Sukanya Chakrabarti (RIT) and collaborators. Search for the
Galaxy_X_(galaxy)
Variable star in the constellation Taurus
photoelectric data by E. F. Guinan in 1966 suggested this is instead a cepheid-type variable with a short pulsation period of about 2.105 days. He refined this
EU_Tauri
Star in the constellation Piscis Austrinus
Austrini is a variable star, and if it is variable, what type of variable star it is. In 1965 it was designated a classical Cepheid variable star with a
Pi_Piscis_Austrini
there are over 52,011 known variable stars, with more being discovered regularly, so a complete list of every single variable is impossible at this place
List_of_variable_stars
Type of star larger than main-sequence but smaller than a giant
this includes Delta Scuti variables such as β Cas. At higher masses the stars would pulsate as Classical Cepheid variables while crossing the instability
Subgiant
Nuclear explosion in a white dwarf star
of novae are classical novae, recurrent novae (RNe), and dwarf novae. They are all considered to be cataclysmic variable stars. Classical nova eruptions
Nova
Astronomical observatory in Massachusetts, US
example, discovered the so-called period-luminosity relation for Classical Cepheid variable stars, establishing the first major "standard candle" with which
Harvard–Smithsonian Center for Astrophysics
Harvard–Smithsonian_Center_for_Astrophysics
Creation of chemical elements within stars
important consequence of blue loops is that they give rise to classical Cepheid variables, of central importance in determining distances in the Milky
Stellar_nucleosynthesis
Speculative physics theory
rate of pulsation of over a thousand cepheid variable stars in 25 galaxies. Theory suggests that the rate of cepheid pulsation in galaxies screened from
Fifth_force
Constellation in the Southern Celestial Hemisphere
Classical Cepheid variable ranging between magnitude 8.88 and 9.82 over 5.9 days. U Antliae is a red C-type carbon star and is an irregular variable that
Antlia
Spiral galaxy in the constellation Ursa Major
light years) by using the Hubble Space Telescope to identify classical Cepheid variables and measure their periods using the period-luminosity relation
Messier_81
Zodiac constellation straddling the celestial equator
number of Cepheid variables, which are used as standard candles to determine astronomical distances. Because of this, astronomers used several Cepheid variables
Virgo_(constellation)
Millikan Classical-map hypernetted-chain method Classical Cepheid Classical Cepheid variable Classical Cepheids Classical Heisenberg model Classical Mechanics
Index_of_physics_articles_(C)
Constellation near the celestial equator
supergiant star, 1200 light-years from Earth. Among the brightest Cepheid variable stars, it has a minimum magnitude of 4.4 and a maximum magnitude of
Aquila_(constellation)
Star in the constellation Carina
variable star in 1981, listed in the General Catalogue of Variable Stars as a possible δ Cephei variable. It has been described as a pseudo-Cepheid,
V382_Carinae
Canadian astronomer
Wayback Machine Turner, David G. (1996). "The Progenitors of Classical Cepheid Variables". Journal of the Royal Astronomical Society of Canada. 90: 82
David_G._Turner
Portion of the giant branch before helium ignition
the instability strip more than once and pulsate as Type I (Classical) Cepheid variables. The table below shows the typical lifetimes on the main sequence
Red-giant_branch
Satellite galaxy of the Milky Way
Solar System. However, in 1986, Caldwell and Coulson found that field Cepheid variables in the northeast lie closer to the Milky Way than those in the southwest
Large_Magellanic_Cloud
Study of oscillations in stars
the pulsations in many of the longest-known variable stars, including the Cepheid and RR Lyrae variables. In stars with surface convection zones, turbulent
Asteroseismology
Constellation in the northern celestial hemisphere
the constellation, is a yellow-white supergiant and the brightest Cepheid variable star in the night sky, ranging in apparent magnitude from 1.97 to 2
Ursa_Minor
Binary star in the constellation Cygnus
fusing heavier elements. Yellow supergiants are usually variable, often Classical Cepheid variables, but 35 Cyg is notable for having an especially constant
35_Cygni
Constellation in the northern celestial hemisphere
was the shortest known for a classical Cepheid at the time of its discovery. W and S Lyrae are two of the many Mira variables in Lyra. W varies between 7th
Lyra
Catalogue of Variable Stars (GCVS4.2)". Retrieved 10 April 2012. Samus, N. N.; Durlevich, O. V.; et al. (2012). "General Catalog of Variable Stars (GCVS
List_of_stars_in_Cassiopeia
Constellation in the southern celestial hemisphere
unusual cepheid variable which shows strong absorption bands in molecular fragments of C2, ⫶CH and ⋅CN, and has been classified as a carbon cepheid of spectral
Triangulum_Australe
Star in the constellation Gemini
positioned near the instability strip and in 1977 was listed as a candidate cepheid variable star with a luminosity amplitude of 0.086 and a period of 0.7282 days
Omega_Geminorum
August 2019). "A three-dimensional map of the Milky Way using classical Cepheid variable stars". Science. 365 (6452): 478–482. arXiv:1806.10653. Bibcode:2019Sci
2019_in_science
Cause of changes in luminosity in pulsating variable stars
of V magnitude, radial velocity, radius with respect to the minimum radius and effective temperature of a classical Cepheid (δ Ceph) over one period.
Kappa–mechanism
Observation in physical cosmology
the world's most powerful telescope at the time. His observations of Cepheid variable stars in "spiral nebulae" enabled him to calculate the distances to
Hubble's_law
Star in the constellation Pegasus
(1951). "Photoelectric Studies. V. Magnitudes and Colors of Classical Cepheid Variable Stars". Astrophysical Journal. 113: 367. Bibcode:1951ApJ...113
9_Pegasi
Constellation in the southern celestial hemisphere
prominent variable stars in Carina. l Carinae is a Cepheid variable noted for its brightness; it is the brightest Cepheid that is variable to the unaided
Carina_(constellation)
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CLASSICAL CEPHEID-VARIABLE
CLASSICAL CEPHEID-VARIABLE
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CLASSICAL CEPHEID-VARIABLE
CLASSICAL CEPHEID-VARIABLE
CLASSICAL CEPHEID-VARIABLE
CLASSICAL CEPHEID-VARIABLE
CLASSICAL CEPHEID-VARIABLE
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