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Type of variable star
RR Lyrae variables are periodic variable stars, commonly found in globular clusters and other old stellar populations in galaxies. They are used as standard
RR_Lyrae_variable
Star in the constellation Lyra
RR Lyrae is a variable star in the Lyra constellation, figuring in its west near to Cygnus. As the brightest star in its class, it became the eponym for
RR_Lyrae
Constellation in the northern celestial hemisphere
famed Summer Triangle asterism. Beta Lyrae is the prototype of a class of binary stars known as Beta Lyrae variables. These binary stars are so close to
Lyra
Type of variable star that pulsates radially
RR Lyrae variables have short periods and lie on the instability strip where it crosses the horizontal branch. Delta Scuti variables and RR Lyrae variables
Cepheid_variable
Stage of stellar evolution
pulsating horizontal-branch stars are known as RR Lyrae variable stars and they are obviously variable in brightness with periods of up to 1.2 days. It
Horizontal_branch
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
Variation in period and amplitude in RR Lyrae type variable stars
long-period modulation, is a variation in period and amplitude in RR Lyrae type variable stars. Sergey Blazhko first reported its observation in 1907 in
Blazhko_effect
Hot, giant star of early spectral type
RR Lyrae variable stars, usually with spectral types of A, lie across the middle of the horizontal branch. Horizontal-branch stars hotter than the RR
Blue_giant
Star in the constellation Andromeda
SW Andromedae is a variable star in the constellation of Andromeda. It is classified as an RR Lyrae star, and varies from an apparent magnitude of 10.09
SW_Andromedae
Rotational center of the Milky Way galaxy
the distance to the Galactic Center as established from variable stars (e.g. RR Lyrae variables) or standard candles (e.g. red-clump stars) is hindered
Galactic_Center
Stellar stream in the constellatiion Virgo discovered in 2005
Hato National Astronomical Observatory in Venezuela to search for RR Lyrae variable stars. Five were found in a clump with a right ascension near 12.4 hours
Virgo_Stellar_Stream
Constellation split into two non-contiguous parts
approximately 25,000 ly distant. Messier 5 contains a large number of known RR Lyrae variable stars, and is receding from us at over 50 km/s. The cluster contains
Serpens
Star whose brightness fluctuates, as seen from Earth
they are at a very different stage of their lives. RR Lyrae variables These relatively common variable stars are somewhat similar to Cepheids, but are not
Variable_star
Variable star
Majoris is a variable star in the northern circumpolar constellation of Ursa Major. It is classified as a Bailey-type 'ab' RR Lyrae variable with a period
TU_Ursae_Majoris
Globular cluster in the constellation Canes Venatici
Way. It contains 274 known variable stars, by far the most found in any globular cluster. These include 133 RR Lyrae variables, of which about a third display
Messier_3
Variable star
MACHO 176.18833.411 (OGLE BLG-RRLYR-10353) is an RR Lyrae variable star located in the galactic bulge of our Milky Way Galaxy. However, it is not a galactic
MACHO_176.18833.411
Type of variable star
and whose present variability is approximately 0.05 of a magnitude. RR Lyrae variable Stellar pulsation Type II Cepheid Soszyński, I.; Pietrukowicz, P.;
Classical_Cepheid_variable
Region of an astronomical diagram
pulsating variable stars: Delta Scuti variables, SX Phoenicis variables, and rapidly oscillating Ap stars (roAps) near the main sequence; RR Lyrae variables where
Instability_strip
Variable star in the constellation Ara
S Arae (S Ara) is an RR Lyrae-type pulsating variable star in the constellation of Ara. It has an apparent visual magnitude which varies between 9.92 and
S_Arae
Globular cluster in the constellation Hercules
with longer period RR Lyrae variable stars. The 1997 Catalogue of Variable Stars in Globular Clusters listed 28 candidate variable stars in the cluster
Messier_92
Globular cluster in the constellation Sagittarius
yet. The mass density at the core is 7.9×104 M☉·pc−3. There are 38 RR Lyrae variable stars and the cluster appears to be Oosterhoff-intermediate in terms
Messier_75
Star in the constellation Lyra
Lyrae, Latinized from ζ1 Lyrae, is the star's Bayer designation. On the island of Kapingamarangi, an asterism of Vega, δ Lyrae, ε Lyrae, and ζ Lyrae is
Zeta1_Lyrae
Constellation straddling the celestial equator
multiple different types of variable stars. M62 is a globular cluster rich in variable stars such as RR Lyrae variables and has two generations of stars
Ophiuchus
Spherical collection of stars
scientific papers. He examined the clusters' RR Lyrae variables (stars which he assumed were Cepheid variables) and used their luminosity and period of variability
Globular_cluster
Globular cluster in the constellation Aquarius
of type ab RR Lyrae variable stars of the cluster. A cluster metallicity below −1.6, an age above 13 billion years, and an average RRab Lyrae pulsation
Messier_2
Multiple star system in the constellation of Lyra
Beta Lyrae (β Lyrae, abbreviated Beta Lyr, β Lyr) officially named Sheliak (Arabic: الشلياق, Romanization: ash-Shiliyāq) (IPA: /ˈʃiːliæk/), the traditional
Beta_Lyrae
Globular cluster in the constellation Ophiuchus
identified 245 variable stars in the cluster's field, of which 209 are RR Lyrae variables, four are Type II Cepheids, 25 are long period variables, and one
Messier_62
Constellation in the northern celestial hemisphere
Sun's, on average, 1.5 M☉. BL Boötis type stars are a subtype of RR Lyrae variables. T Boötis was a nova observed in April 1860 at a magnitude of 9.7
Boötes
Globular cluster in Ophiuchus
stellar population includes four Cepheids and RV Tauri variables, plus at least one RR Lyrae variable for which a period is known. Observations made during
Messier_19
Star in the constellation Lyra
R Lyrae, also known by its Flamsteed designation 13 Lyrae and named Niandao, is a 4th magnitude semiregular variable star in the constellation Lyra, approximately
R_Lyrae
Astronomical principle
The cluster variables (RR Lyrae variables) were fainter still. Period-luminosity relations are known for several types of pulsating variable stars: type
Period-luminosity_relation
Spheroidal galaxy in the constellation Draco
discovered over 260 variables. Of the 138 in the cluster's center, all but five were determined to be RR Lyrae variables. From this work a RR Lyrae derived distance
Draco_Dwarf
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
Brightest star in the constellation Lyra
constellation of Lyra. It has the Bayer designation α Lyrae, which is Latinised to Alpha Lyrae and abbreviated Alpha Lyr or α Lyr. This star is relatively
Vega
Globular cluster
helium burning horizontal branch (HB) stars, including at least one RR Lyrae variable star. Terzan 5 is known to contain 49 millisecond radio pulsars as
Terzan_5
2015, strange nonchaotic dynamics were identified for the pulsating RR Lyrae variable KIC 5520878, as well as three similar stars observed by the Kepler
Strange_nonchaotic_attractor
B. B.; et al. (August 1977), "Photoelectric UBV observations of RR Lyrae variable stars. Second list", Revista Mexicana de Astronomía y Astrofísica
List of star systems within 60–65 light-years
List_of_star_systems_within_60–65_light-years
Globular cluster in Ophiuchus
the galactic bar. There are 22 known RR Lyrae variable stars in this cluster and a probable SX Phoenicis variable. List of Messier objects Shapley, Harlow;
Messier_107
Globular cluster in the constellation Dorado
on 20 December 1835. NGC 1786 has 65 variable stars that have been identified. Among them are 53 RR Lyrae variables, along with 3 classical Cepheids, a
NGC_1786
Constellation in the southern celestial hemisphere
populations of the Milky Way. Investigation of the area yielded only ten RR Lyrae variables—consistent with the Milky Way's halo and thick disk populations rather
Canis_Major
Globular cluster in Ophiuchus
sized telescopes. There have been 24 variable stars found in M9: 21 RR Lyrae variables, plus a long-period variable, Type II Cepheid, and an eclipsing binary
Messier_9
Disputed galaxy located near the constellation Canis Major
spheroidal galaxy. Investigation of the area in 2009 yielded only ten RR Lyrae variable stars, consistent with the Milky Way's halo and thick disk populations
Canis_Major_Overdensity
Globular star cluster in the constrellation Hydrus
RR Lyrae variable stars in the cluster, as of 2011. Eight are RRd, or double-mode RR Lyrae variables. The average periods are 0.591 days for RR Lyrae
NGC_1466
Globular cluster in the constellation Sagitta
usual for an ancient globular cluster; furthermore, it lacks the RR Lyrae "cluster" variable stars that are common in most globular clusters. However, modern
Messier_71
Globular cluster in the constellation Tucana
This suggests the later generation is more centrally concentrated. RR Lyrae variable stars were detected in this cluster in 1988. 20 candidate Dwarf Cepheid
NGC_121
Scatter plot of stars showing the relationship of luminosity to stellar classification
luminosities. RR Lyrae variable stars are horizontal-branch stars in a section of the diagram called the instability strip. Cepheid variables also fall on
Hertzsprung–Russell_diagram
American astronomer
astronomer specializing in the observation of variable stars and recognized as an expert on RR Lyrae variable stars. She became known for her work as the
Emilia_Pisani_Belserene
Cause of changes in luminosity in pulsating variable stars
there are negative hydrogen ions. An example of such a zone is in RR Lyrae variables where the partial second ionization of helium occurs. Hydrogen ionization
Kappa–mechanism
Variable star in the constellation of Lynx
may be the result of shockwaves that increase light emission. As an RR Lyrae variable, AI Velorum should be a low mass, evolved star. However, M. Breger
AI_Velorum
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
Binary star system in the constellation of Lyra
originally included this as a candidate member of the proposed Delta Lyrae cluster. The variable radial velocity of this star was discovered from photographic
Delta1_Lyrae
Globular cluster in the constellation Centaurus
RR Lyrae Variables G III F III A III Blue Stragglers A V B V SX Phoenicis Variables A V F V BY Draconis Variables G V K V M V Cataclysmic Variables K
Omega_Centauri
Constellation in the northern hemisphere
and 5.3. R Comae Berenices is a Mira variable with a maximum magnitude of almost 7. There are 123 RR Lyrae variables in the constellation, with many in
Coma_Berenices
Globular cluster in the constellation Coma Berenices
There are ten known RR Lyrae variable stars in this cluster with masses ranging from 68% to 78% of the solar mass. Nine of these variables were reported by
NGC_5053
Multiple star system in the constellation of Lyra
Epsilon Lyrae (ε Lyr, ε Lyrae) is a multiple star system of at least five stars approximately 160 light-years away in the constellation of Lyra. It is
Epsilon_Lyrae
Dutch astronomer (1904–1978)
populations of globular clusters based on the periodicities of their RR Lyrae variable stars. These two populations would come to be known as Oosterhoff
Pieter_Oosterhoff
Dwarf spheroidal galaxy in the constellation Andromeda
from the center of M31. A total of 56 variable stars have been discovered in And III, including 51 RR Lyrae variables. List of Andromeda's satellite galaxies
Andromeda_III
Succession of methods by which astronomers determine the distances to celestial objects
are in an older stellar population (like novae and RR Lyrae variables) must be used. RR Lyrae variables are less luminous than Cepheids, and novae are unpredictable
Cosmic_distance_ladder
Star in the constellation Lyra
Gamma Lyrae, Latinised from γ Lyrae, and formally named Sulafat /ˈsuːləfæt/, is the second-brightest star in the northern constellation of Lyra. With
Gamma_Lyrae
Globular cluster in Scorpius
7.1 ly (2.18 pc). This cluster has an abnormally large number of RR Lyrae variables—68 candidates as of 2006, and their periods are longer than is typical
NGC_6441
Star in the constellation Boötes
the variable star designation BL Boötis. However, he thought it was an eclipsing binary. It was subsequently thought to be an RR Lyrae variable by T
BL_Boötis
Globular cluster in the constellation Ophiuchus
parsec. 35 variable stars have been discovered in this cluster, including one RR Lyrae variable, two eclipsing binaries, three W Virginis variables, five semiregular
Messier_10
Overview of the scientific field of astronomy
astronomy Variable star Pulsating Cepheids and cepheid-like Cepheid variable Type II Cepheids RR Lyrae variable Delta Scuti variable SX Phoenicis variable Blue-white
Outline_of_astronomy
Globular cluster
radius of 189 light years. VVV CL160 has a significant population of RR Lyrae variable stars. This globular cluster has an unusually high proper motion when
VVV_CL160
Globular cluster in the constellation Coma Berenices
stream. Among the variable star population in the cluster, there are 55 RR Lyrae variables. There are also at least three variables of type SX Phe and
Messier_53
Variable star in the constellation Virgo
type. The light curve is asymmetrical, resembling that of a type ab RR Lyrae variable. On the HR diagram it is positioned above the horizontal branch. For
XX_Virginis
Globular cluster in the constellation Serpens
there are 105 known variable stars, 97 of them belonging to the RR Lyrae type. RR Lyrae stars, sometimes referred to as "Cluster Variables", are somewhat similar
Messier_5
Dwarf galaxy in the constellation Fornax
have horizontal branches across a wide range of colors and include RR Lyrae variables, Fornax 4 is found to have only red in its horizontal branch. Fornax
Fornax_Dwarf
; Johnson, H. L. (1977-08-01). "Photoelectric UBV observations of RR Lyrae variable stars. Second list". Revista Mexicana de Astronomía y Astrofísica
List_of_nearest_giant_stars
Astrometry Parallax Parallax in astronomy Stellar parallax Cepheid Stars RR Lyrae Variable Stars Mamajek (2005). "A Moving Cluster Distance to the Exoplanet
Moving-cluster_method
Globular cluster in the constellation Coma Berenices
has the lowest metallicity of any OoI cluster known. There are 19 RR Lyrae variable star candidates and as many as 23 blue stragglers. A high proportion
NGC_4147
Dwarf spheroidal galaxy in the constellation Andromeda
And II have ages between 6 and 9 Gyr. However, the observation of RR Lyrae variables and blue horizontal-branch stars demonstrates the existence of a population
Andromeda_II
Globular cluster in the constellation Telescopium
least 69 variable stars, most of which are RR Lyrae variables: 46 stars were identified as RRab variables; 15 as RRc variables, 1 RRe variable, 4 eclipsing
NGC_6584
Type of variable star
the Hertzsprung–Russell diagram they fall in-between W Virginis and RR Lyrae variables. The prototype star, BL Herculis, varies between magnitude 9.7 and
BL_Herculis_variable
Galaxy in the constellation Leo
giants, although a number of Horizontal branch stars including three RR Lyrae variable stars were also discovered. The stars of Leo IV were probably among
Leo_IV_(dwarf_galaxy)
Variable star in the constellation of Lynx
of 0.25 days. H. Schneller in 1961 classified it as a short-period RR Lyrae variable. O. J. Eggen in 1962 found a period of 0.12 days, or half that of
SZ_Lyncis
Grouping of evolved cool luminous stars
circulate core material to the surface. AGB stars are typically long-period variables, and suffer mass loss in the form of a stellar wind. For M-type AGB stars
Asymptotic_giant_branch
Globular cluster in Scorpius
age of the globular cluster NGC 6121 (M4) from the properties of RR Lyrae variables". Astronomy and Astrophysics. 143 (1): 8–12. Bibcode:1985A&A...143
Messier_4
Red giant star in the constellation Lyra
It is a semi-regular variable star that has its brightness change by 0.2 magnitudes over an ill-defined period. Delta2 Lyrae was a 5.0 M☉ star when
Delta2_Lyrae
Globular cluster in the constellation Horologium
total of 22 RR Lyrae variables have been discovered in this cluster, along with two long-period variables, three SX Phoenicis variables, and an eclipsing
NGC_1261
Binary star system in the globular cluster of Messier 4
age of the globular cluster NGC 6121 (M4) from the properties of RR Lyrae variables". Astronomy and Astrophysics. 143 (1): 8–12. Bibcode:1985A&A...143
PSR_B1620−26
Astronomical survey program
(IPAC). Studies included compact binaries (AM CVn stars), RR Lyrae, cataclysmic variables, and active galactic nuclei (AGN), and lightcurves of small
Palomar_Transient_Factory
Changes to stars over their lifespans
becoming unstable pulsating stars in the yellow instability strip (RR Lyrae variables), whereas some become even hotter and can form a blue tail or blue
Stellar_evolution
Star in the constellation Lyra
Eta Lyrae, a name Latinized from η Lyrae, is a likely binary star system in the northern constellation of Lyra. It has the traditional name Aladfar /əˈlædfɑːr/
Eta_Lyrae
Fluctuations in stellar radius
Doppler effect. Many intrinsic variable stars that pulsate with large amplitudes, such as the classical Cepheids, RR Lyrae stars and large-amplitude Delta
Stellar_pulsation
Variable star in the constellation Ursa Major
Hoffmeister announced his discovery of this variable star, in 1963. He erroneously classified it as an RR Lyrae variable. This is a single-lined spectroscopic
AN_Ursae_Majoris
Catalogue of Variable Stars (GCVS4.2)". Retrieved 3 April 2012. Samus, N. N.; Durlevich, O. V.; et al. (2012). "General Catalog of Variable Stars (GCVS
List_of_stars_in_Caelum
Star in the constellation Pegasus
instead be a high amplitude Delta Scuti variable. The short period of this variable rules it out as an RR Lyrae variable. The properties of DY Pegasi are uncertain
DY_Pegasi
Irregular galaxy in the Local Group
suggesting a rather unusual evolutionary history. The presence of RR Lyrae variables shows that the galaxy has an old stellar population that is up to
Leo_A
Single, yellow-white hued star in the constellation Eridanus
amplitude Delta Scuti variable with a primary period of 0.273 days. It was originally classified, tentatively, as an RR Lyrae variable of type 'c'. 64 Eridani
64_Eridani
Variable star in the constellation Cancer
classified as a cluster-type Cepheid variable, or RR Lyrae star. In 1955, W. S. Fitch found the light curve to be variable and discovered a beat period of
VZ_Cancri
2008). "The Luminosities and Distance Scales of Type II Cepheid and RR Lyrae variables". Monthly Notices of the Royal Astronomical Society. 386 (4): 2115–2134
List_of_nearest_supergiants
Star in the southern constellation of Puppis
B. B.; et al. (August 1977), "Photoelectric UBV observations of RR Lyrae variable stars. Second list", Revista Mexicana de Astronomía y Astrofísica
Rho_Puppis
Complex, ringlike filament of stars wrapped around the Milky Way
main stellar disk, with the velocity dispersion of their constituent RR Lyrae variable stars found to be higher and consistent with halo membership. Using
Monoceros_Ring
Discredited cosmological model, early 20th Century
period was established by Henrietta Leavitt in 1908. Using cepheid and RR Lyrae variables to systematically chart the distribution of globular clusters, Shapley
Galactocentrism
Globular cluster in the constellation Columba
binary pulsars, of which six are MSPs and one is mildly recycled. 43 RR Lyrae variables have been discovered in the cluster, which show this to be an Oosterhoff
NGC_1851
Star in the constellation Triangulum Australe
It was first discovered to be variable by Annie Jump Cannon in 1910 and initially classified as an RR Lyrae variable. Later authors segregated it and
RT_Trianguli_Australis
Globular cluster in the constellation Sagittarius
generations of stars. Five known variable stars lie within its broadest radius, the tidal radius, all of which are RR Lyrae variables. The cluster may have two
Messier_70
Canadian-American physicist (1916–2012)
Christy began an investigation of Cepheid variables and the smaller RR Lyrae variables, classes of luminous variable stars. At the time it was a mystery as
Robert_F._Christy
Variable Star Observers. Retrieved 9 March 2014. E.B Knobel – On a catalogue of stars in the Calendarium of Al Achsasi Al Mouakket Labelled Pi Lyrae (π
List_of_stars_in_Lyra
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