46 relations: Alpha Herculis, American Association of Variable Star Observers, Apparent magnitude, Asymptotic giant branch, Beta Gruis, Betelgeuse, Carbon star, Centre de données astronomiques de Strasbourg, Cepheid variable, Day, Eta Geminorum, General Catalogue of Variable Stars, Gravitational microlensing, HD 3346, Hypergiant, International Astronomical Union, L2 Puppis, Large Magellanic Cloud, Light curve, List of semiregular variable stars, Long-period variable star, Low-dimensional chaos in stellar pulsations, Mira variable, Mu Cephei, Normal mode, Omicron1 Centauri, Optical Gravitational Lensing Experiment, Overtone, Pi1 Gruis, Red giant, Rho Cassiopeiae, Rho Persei, RR Coronae Borealis, RV Tauri variable, RW Cygni, S Vulpeculae, S-type star, Sigma Librae, Slow irregular variable, Stellar classification, Supergiant star, T Centauri, UU Aurigae, V509 Cassiopeiae, Variable star designation, 15 Arietis.
Since its founding in 1911, the American Association of Variable Star Observers (AAVSO) has coordinated, collected, evaluated, analyzed, published, and archived variable star observations made largely by amateur astronomers and makes the records available to professional astronomers, researchers, and educators.
The apparent magnitude of a celestial object is a number that is a measure of its brightness as seen by an observer on Earth.
The asymptotic giant branch (AGB) is a region of the Hertzsprung–Russell diagram populated by evolved cool luminous stars.
Beta Gruis (β Gruis, abbreviated Bet Gru, β Gru), also named Tiaki, is the second brightest star in the southern constellation of Grus.
Betelgeuse, also designated Alpha Orionis (α Orionis, abbreviated Alpha Ori, α Ori), is the ninth-brightest star in the night sky and second-brightest in the constellation of Orion.
A carbon star is typically an asymptotic giant branch star, a luminous red giant, whose atmosphere contains more carbon than oxygen; the two elements combine in the upper layers of the star, forming carbon monoxide, which consumes all the oxygen in the atmosphere, leaving carbon atoms free to form other carbon compounds, giving the star a "sooty" atmosphere and a strikingly ruby red appearance.
The Centre de Données astronomiques de Strasbourg (CDS; English translation: Strasbourg Astronomical Data Center) is a data hub which collects and distributes astronomical information.
A Cepheid variable is a type of star that pulsates radially, varying in both diameter and temperature and producing changes in brightness with a well-defined stable period and amplitude.
A day, a unit of time, is approximately the period of time during which the Earth completes one rotation with respect to the Sun (solar day).
Eta Geminorum (η Geminorum, abbreviated Eta Gem, η Gem), also named Propus, is a triple star system in the constellation of Gemini.
The General Catalogue of Variable Stars (GCVS) is a list of variable stars.
Gravitational microlensing is an astronomical phenomenon due to the gravitational lens effect.
HD 3346, also known as V428 Andromedae, is an orange giant star approximately 620 light-years away in the constellation of Andromeda.
A hypergiant (luminosity class 0 or Ia+) is among the very rare kinds of stars that typically show tremendous luminosities and very high rates of mass loss by stellar winds.
The International Astronomical Union (IAU; Union astronomique internationale, UAI) is an international association of professional astronomers, at the PhD level and beyond, active in professional research and education in astronomy.
L2 Puppis (also known as HD 56096) is a giant star in the constellation of Puppis and is located between the bright stars Canopus and Sirius.
The Large Magellanic Cloud (LMC) is a satellite galaxy of the Milky Way.
In astronomy, a light curve is a graph of light intensity of a celestial object or region, as a function of time.
This is a list of semiregular variable stars.
The descriptive term long-period variable star refers to various groups of cool luminous pulsating variable stars.
Low-dimensional chaos in stellar pulsations is the current interpretation of an established phenomenon.
Mira variables ("Mira", Latin, adj. - feminine form of adjective "wonderful"), named for the prototype star Mira, are a class of pulsating variable stars characterized by very red colours, pulsation periods longer than 100 days, and amplitudes greater than one magnitude in infrared and 2.5 magnitude at visual wavelengths.
Mu Cephei (μ Cep, μ Cephei), also known as Herschel's Garnet Star, is a red supergiant star in the constellation Cepheus.
A normal mode of an oscillating system is a pattern of motion in which all parts of the system move sinusoidally with the same frequency and with a fixed phase relation.
Omicron1 Centauri (ο1 Cen, ο1 Centauri) is a star in the constellation Centaurus.
The Optical Gravitational Lensing Experiment (OGLE) is a Polish astronomical project based at the University of Warsaw that runs a long-term variability sky survey (1992-present).
An overtone is any frequency greater than the fundamental frequency of a sound.
π1 Gruis (Pi1 Gruis) is a semiregular variable star in the constellation Grus around 530 light-years from Earth.
A red giant is a luminous giant star of low or intermediate mass (roughly 0.3–8 solar masses) in a late phase of stellar evolution.
Rho Cassiopeiae (ρ Cas, ρ Cassiopeiae) is a yellow hypergiant star in the constellation Cassiopeia.
Rho Persei (Rho Per, ρ Persei, ρ Per) is a star in the northern constellation of Perseus.
RR Coronae Borealis (RR CrB, HD 140297, HIP 76844) is a M3-type semiregular variable star located in the constellation Corona Borealis with a parallax of 2.93mas being a distance of.
RV Tauri variables are luminous variable stars that have distinctive light variations with alternating deep and shallow minima.
RW Cygni is a semiregular variable star in the constellation Cygnus, about a degree east of 2nd magnitude γ Cygni.
S Vulpeculae is a star located in the constellation Vulpecula.
An S-type star (or just S star) is a cool giant with approximately equal quantities of carbon and oxygen in its atmosphere.
Sigma Librae (σ Librae, abbreviated Sig Lib, σ Lib) is a binary star in the constellation of Libra.
A slow irregular variable (ascribed the GCVS types L, LB and LC) is a variable star that exhibit no or very poorly defined periodicity in their slowly changing light emissions.
In astronomy, stellar classification is the classification of stars based on their spectral characteristics.
Supergiants are among the most massive and most luminous stars.
T Centauri is a variable star located in the far southern constellation Centaurus.
UU Aurigae is a carbon star and binary star in the constellation Auriga.
V509 Cassiopeiae (V509 Cas or HR 8752) is one of two yellow hypergiant stars found in the constellation Cassiopeia, which also contains Rho Cassiopeiae.
Variable stars are designated using a variation on the Bayer designation format of an identifying label (as described below) combined with the Latin genitive of the name of the constellation in which the star lies.
15 Arietis (abbreviated 15 Ari) is a single variable star in the northern constellation of Aries.
Mu Cephei variable, SR Variable, SR variable, SRA variable, SRB variable, SRC variable, SRD variable, Semi-regular variable, Semi-regular variable star, Semiregular variable, Semiregular variable stars, Semiregular variables, UU Herculis variable.