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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
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
Northern pole-star; brightest star in Ursa Minor
Aa/Ab pair only confirmed in the early 20th century. As the closest Cepheid variable, Polaris Aa's distance is a foundational part of the cosmic distance
Polaris
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
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
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
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
Eclipsing contact binary in Holmberg IX
Majoris variable. The data from the Large Binocular Telescope for Holmberg IX V1 could also fit a massive long-period Cepheid variable with a variable period
Holmberg_IX_V1
Star whose brightness fluctuates, as seen from Earth
numerous observations of variable stars, paying particular attention to Cepheid variables. Her analyses and observations of variable stars, carried out with
Variable_star
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
Succession of methods by which astronomers determine the distances to celestial objects
of distance measurements using Cepheid variables. In the 1950s, Walter Baade discovered that the nearby Cepheid variables used to calibrate the standard
Cosmic_distance_ladder
American astronomer (1868–1921)
relationship she discovered in it, between the period of certain variable stars (Cepheids) and their apparent brightness, reflected a relationship in their
Henrietta_Swan_Leavitt
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
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 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
Barred spiral galaxy in the Local Group
Hubble settled the debate in 1925 when he identified extragalactic Cepheid variable stars for the first time on astronomical photos of Andromeda. These
Andromeda_Galaxy
Constellation in the southern celestial hemisphere
origins and motion across the southern Milky Way. Crux contains four Cepheid variables, each visible to the naked eye under optimum conditions. Crux also
Crux
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
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 star
SU_Cygni
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
Constellation in the northern celestial hemisphere
Delta Cephei is the prototype of an important class of star known as a Cepheid variable. RW Cephei, an orange hypergiant, together with the red supergiants
Cepheus_(constellation)
Topics referred to by the same term
A Cepheid is a type of pulsating variable star. It may also refer to: Cepheid (company), a molecular diagnostics company Cepheid, a fictional alien species
Cepheid_(disambiguation)
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
Dwarf irregular galaxy, satellite galaxy of the Milky Way
distance to any other Cepheid variable to be estimated in terms of the distance to the SMC. She hoped a few Cepheid variables could be found close enough
Small_Magellanic_Cloud
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 that has a supergiant luminosity class, with a spectral type of F or G
Delta Canis Majoris and Iota¹ Scorpii. Many of them are variable stars, mostly pulsating Cepheids such as δ Cephei itself. Hertzsprung–Russell diagram Spectral
Yellow_supergiant
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
Variable star in the constellation Cygnus
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 period
V1334_Cygni
Galaxy containing the Solar System
estimate from 1997 by Goodwin and others compared the distribution of Cepheid variable stars in 17 other spiral galaxies to the ones in the Milky Way, and
Milky_Way
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
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)
Type of star that is massive and luminous
study of Cepheid variables". Popular Astronomy. 34: 493. Bibcode:1926PA.....34..493H. Shapley, Harlow (1925). "S Doradus, a Super-giant Variable Star".
Supergiant
Region of an astronomical diagram
intersects the horizontal branch; and the Cepheid variables where it crosses the supergiants. RV Tauri variables are also often considered to lie on the
Instability_strip
Student-run convention at Texas A&M University
multigenre convention in the United States. Held annually since 1969 by Cepheid Variable at Texas A&M University's Memorial Student Center, it has grown to
AggieCon
Two dwarf galaxies orbiting the Milky Way
in 1913 using 1912 measurements of Cepheid variables in the SMC by Henrietta Leavitt. Recalibration of the Cepheid scales allowed Harlow Shapley to refine
Magellanic_Clouds
Repetitive variation of some measure about a central value
periodic firing of nerve cells in the brain, and the periodic swelling of Cepheid variable stars in astronomy. The term vibration is precisely used to describe
Oscillation
Type of variable star
not be confused with Cepheid variables, which are named after Delta Cephei and are luminous supergiant stars. Beta Cephei variables are somewhat evolved
Beta_Cephei_variable
Zodiac constellation in the northern hemisphere
small telescopes. ζ Gem (Mekbuda) is a double star, whose primary is a Cepheid variable star with a period of 10.2 days; its minimum magnitude is 4.2 and its
Gemini_(constellation)
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 Swan
Edwin_Hubble
Increase in distance between parts of the universe
Cluster more closely agree with subsequent and independent analyses of Cepheid variable calibrations of Type Ia supernovae, which estimates a Hubble constant
Expansion_of_the_universe
Scientific study of celestial objects
demonstrated in the 20th century. In 1912, Henrietta Leavitt discovered Cepheid variable stars with well-defined, periodic luminosity changes which can be used
Astronomy
American scientist and political activist (1885–1972)
political activist during the New Deal and Fair Deal. Shapley used Cepheid variable stars to estimate the size of the Milky Way Galaxy and the Sun's position
Harlow_Shapley
first candidate to be a lensed yellow supergiant star, and possibly a Cepheid variable. List of most distant stars Diego, J. M.; Palencia, J. M.; Goolsby
Hedorah_(star)
Star in the constellation Gemini
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 its
Zeta_Geminorum
Methods for estimating the age of a star
tracked in its evolutionary path, one can estimate the age of the Cepheid variable. Exceptional stellar properties which allow for an estimation of age
Stellar_age_estimation
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
Star in the constellation Camelopardalis
Virginis variable (type II Cepheid) in the constellation of Camelopardalis. It is also a carbon star, which is very unusual for a Cepheid variable. RU Cam
RU_Camelopardalis
Constellation in the northern celestial hemisphere
magnitude of −5.7. It lies 3,976 light-years from Earth. RT Aurigae is a Cepheid variable which ranges between magnitudes 5.0 and 5.8 over a period of 3.7 days
Auriga
Variable star in the constellation Crux
S Crucis is a star in the constellation Crux. A Cepheid variable, its apparent magnitude ranges from 6.22 to 6.92 over 4.68997 d. It is a yellow-white
S_Crucis
Hungarian astronomer
eclipsing stars, and the observation of convection within V1154 Cyg, a Cepheid variable star. Derekas completed a Ph.D. in 2009 at the University of Sydney
Aliz_Derekas
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 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
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. P. Kraft
X_Cygni
(July 2018). "The Araucaria Project: High-precision Cepheid Astrophysics from the Analysis of Variables in Double-lined Eclipsing Binaries". The Astrophysical
List_of_nearest_supergiants
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
Galaxy in the constellation Coma Berenices
its Cepheid variable stars. The outer arms appear blue due to the continuing formation of young stars and include a possible luminous blue variable with
NGC_4414
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
Variable star in the Large Magellanic Cloud
eclipsing binary and Cepheid variable star, pulsating every 3.8 days. The star, in the Large Magellanic Cloud, was the first Cepheid star system found to
OGLE-LMC-CEP0227
Galaxy in the constellation Canes Venatici
contains Cepheid variables similar to both the metallicities of the Milky Way and other galaxies' Cepheids. By measuring the distance of the Cepheids with
Messier_106
Star in the constellation Auriga
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 3.728309
RT_Aurigae
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
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
Variable star in the constellation Pavo
was κ Pav was listed as a likely Cepheid variable. In 1937 it was used as part of the effort to calibrate the Cepheid distance scale. Only years later
Kappa_Pavonis
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 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
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. Based
Beta_Doradus
Multiple star in the constellation Aquila
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
Spectroscopic binary star system in the constellation Scorpius
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
through parallax measurements, use of standard references such as cepheid variables or Type Ia supernovas to the object in which the star resides, or
List_of_most_distant_stars
Technique in stellar astrophysics
Baade-Wesselink method is a method for determining the distance of a Cepheid variable star suggested by Walter Baade in 1926 and further developed by Adriaan
Baade-Wesselink_method
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
Open cluster in the constellation Scutum
and later observed by his son, John Herschel. NGC 6664 is home to 16 Cepheid variable stars. 11 are B type, the remaining five are red giants. NGC 6664 contains
NGC_6664
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 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 a period
BG_Crucis
Class of luminous variable star
instability strip. Therefore, RV Tau variables along with W Vir variables are sometimes considered a subclass of Type II Cepheids. They exhibit relationships between
RV_Tauri_variable
Constellation in the southern celestial hemisphere
magnitude of 3.19. Slightly variable, it is the brightest rapidly oscillating Ap star in the night sky. AX Circini is a Cepheid variable visible with the unaided
Circinus
Large, comparatively empty region of space
measurements of the Hubble constant using galactic supernovae and Cepheid variables (72–75 km/s/Mpc) and the cosmic microwave background and baryon acoustic
Local_Hole
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)
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)
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
Open cluster in the constellation Cassiopeia
of the cluster is DL Cassiopeiae, a binary system which contains a Cepheid variable with a 8,00 day period. Using the fluctuations of the brightness of
NGC_129
Constellation in the southern sky
is the brightest star in Dorado. Beta Doradus is a notably bright Cepheid variable star. It is a yellow-tinged supergiant star that has a minimum magnitude
Dorado
Astronomical observatory in Los Angeles County, California, US
work on the Hooker telescope. In 1923, Hubble discovered the first Cepheid variable in the spiral nebula of Andromeda using the 2.5-meter telescope. This
Mount_Wilson_Observatory
British astrophysicist (1882–1944)
in 1916 with investigations of possible physical explanations for Cepheid variable stars. He began by extending Karl Schwarzschild's earlier work on radiation
Arthur_Eddington
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
Astronomical phenomenon caused by light reflected off surfaces distant from the source
imposters. Light echoes were used to determine the distance to the Cepheid variable RS Puppis to an accuracy of 1%. Pierre Kervella at the European Southern
Light_echo
Subfield of astronomy
University of Vienna in the late 19th century. Soon after the discovery of Cepheid variable stars, theorists shifted from CM and geodesy to the development of
Astrophysics
Variable star in the constellation Sagitta
also known by the Flamsteed designation of 10 Sagittae, a Classical Cepheid variable in the constellation Sagitta that varies from magnitude 5.24 to 6.04
S_Sagittae
Void between celestial bodies
Pacific, 100: 6–7, Bibcode:1988PASP..100....6C, doi:10.1086/132128. Cepheid Variable Stars & Distance Determination, CSIRO Australia, October 25, 2004,
Outer_space
Type of star that is luminous, blue, and variable in brightness
3 had already been classified as a Cepheid variable. At the time they were simply described as irregular variables, although remarkable for being the
Luminous_blue_variable
Star in the constellation Carina
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 a period
HD_95109
1920 debate between Harlow Shapley and Heber Curtis on whether there were other galaxies
estimates for the size of the Milky Way using globular clusters and the Cepheid variables found within them. He presented the audience with a "universe" 300
Great_Debate_(astronomy)
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
Natural physical entity in space
region of the H-R diagram that includes Delta Scuti, RR Lyrae and Cepheid variables. The evolving star may eject some portion of its atmosphere to form
Astronomical_object
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
American astronomer (1927–2015)
2015) was an American astronomer. He performed pioneering work on Cepheid variables, stellar rotation, novae, and the chemical evolution of the Milky
Robert_Kraft_(astronomer)
Nuclear explosion in a white dwarf star
have been shown to be of comparable accuracy to those measured with Cepheid variable stars. A recurrent nova (RN) is an object that has been seen to experience
Nova
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 Way and
Stellar_nucleosynthesis
Astronomical observatory in Wyoming
main telescope. Research at the observatory has included monitoring Cepheid variable stars and follow-up observation of gamma-ray bursts. Wyoming Infrared
Red_Buttes_Observatory
German astronomer (1893–1960)
same observations led him to discover that there are two types of Cepheid variable stars. Using this discovery he recalculated the size of the known universe
Walter_Baade
CEPHEID VARIABLE
CEPHEID VARIABLE
Girl/Female
Biblical
According to variable songs or tunes.
Biblical
according to variable songs or tunes,
Surname or Lastname
English
English : topographic name for someone living on (and farming) a hide of land, Old English hī(gi)d. This was a variable measure of land, differing from place to place and time to time, and seems from the etymology to have been originally fixed as the amount necessary to support one (extended) family (Old English hīgan, hīwan ‘household’). In some cases the surname is habitational, from any of the many minor places named with this word, as for example Hyde in Greater Manchester, Bedfordshire, and Hampshire.English : variant of Ide, with inorganic initial H-. Compare Herrick.Jewish (American) : Americanized spelling of Haid.
Boy/Male
Greek Latin
The father of Andromeda in ancient Greek mythology.
Boy/Male
Anglo, British, English
Variable
Surname or Lastname
English (of Norman origin)
English (of Norman origin) : habitational name from Saint-Hilaire-du-Harcouët in La Manche, which gets its name from the dedication of its church to St. Hilary, or alternatively from either of the places, in La Manche and Somme, called Saint-Lô. Both of the latter are named from a 6th-century St. Lauto, bishop of Coutances; his name is of variable form in the sources and uncertain etymology.North German : habitational name for someone from Sandel.Jewish (eastern Ashkenazic) : occupational name for a cobbler or shoemaker, Yiddish sandler (from Hebrew sandelar, from Late Latin sandalarius, an agent derivative of sandalium ‘shoe’).
Boy/Male
Anglo, Australian, British, English, French, Swedish
Variable; Brave with the Spear; Spear Rule
Surname or Lastname
English
English : from a medieval male personal name (from Latin Hilarius, a derivative of hilaris ‘cheerful’, ‘glad’, from Greek hilaros ‘propitious’, ‘joyful’). The Latin name was chosen by many early Christians to express their joy and hope of salvation, and was borne by several saints, including a 4th-century bishop of Poitiers noted for his vigorous resistance to the Arian heresy, and a 5th-century bishop of Arles. Largely due to veneration of the first of these, the name became popular in France in the forms Hilari and Hilaire, and was brought to England by the Norman conquerors.English : from the much rarer female personal name Eulalie (from Latin Eulalia, from Greek eulalos ‘eloquent’, literally well-speaking, chosen by early Christians as a reference to the gift of tongues), likewise introduced into England by the Normans. A St. Eulalia was crucified at Barcelona in the reign of the Emperor Diocletian and became the patron of that city. In England the name underwent dissimilation of the sequence -l-l- to -l-r- and the unfamiliar initial vowel was also mutilated, so that eventually the name was considered as no more than a feminine form of Hilary (of which the initial aspirate was in any case variable).
CEPHEID VARIABLE
CEPHEID VARIABLE
Boy/Male
Muslim/Islamic
Praising (Allah)
Boy/Male
Afghan, Arabic, German, Hindu, Indian, Iranian, Muslim, Parsi
Goodness; Compassion; In God Grace; Worthy
Surname or Lastname
English (Cumbria)
English (Cumbria) : variant of Irvin.
Boy/Male
Indian, Sanskrit
With Loud Laughter; Lord Shiva
Boy/Male
Assamese, Hindu, Indian, Marathi
The Healer; Vishnu; Who Cures the Disease of Birth and Death Cycles
Boy/Male
African, American, Arabic, Bengali, French, Hindu, Indian, Iranian, Malaysian, Marathi, Muslim, Oriya, Parsi, Pashtun, Sindhi
Divine Grace; Trustworthy; Honest; Another Name for Prophet Muhammad; Faithful; Custodian; Truthful
Boy/Male
Hindu
Vaishnava denotes Lord Vishnu
Girl/Female
Hindu, Indian, Marathi
White Rays
Boy/Male
Muslim
Shah. King.
Girl/Female
Hindu
CEPHEID VARIABLE
CEPHEID VARIABLE
CEPHEID VARIABLE
CEPHEID VARIABLE
CEPHEID VARIABLE
n.
A shifting wind, or one that varies in force.
a.
Having always the same form, manner, or degree; not varying or variable; unchanging; consistent; equable; homogenous; as, the dress of the Asiatics has been uniform from early ages; the temperature is uniform; a stratum of uniform clay.
n.
One of the external openings communicating with the air tubes or tracheae of insects, myriapods, and arachnids. They are variable in number, and are usually situated on the sides of the thorax and abdomen, a pair to a segment. These openings are usually elliptical, and capable of being closed. See Illust. under Coleoptera.
a.
Liable to be turned in opinion; changeable; variable; unsteady; inconstant; as versatile disposition.
a.
Changeable; uncertain; inconstant; variable.
a.
Changing in place, position, or direction; varying; variable; fickle; as, shifting winds; shifting opinions or principles.
a.
Irresolute; inconsonant; variable; untrustworthy; as, an uncertain person; an uncertain breeze.
a.
Having the capacity of varying or changing; capable of alternation in any manner; changeable; as, variable winds or seasons; a variable quantity.
a.
Varying in from, character, or the like; variable; different; diverse.
n.
The quality or state of being variable; variability.
adv.
In a variable manner.
n.
The quality or state of being variable; variableness.
a.
Liable to vary; too susceptible of change; mutable; fickle; unsteady; inconstant; as, the affections of men are variable; passions are variable.
n.
Those parts of the sea where a steady wind is not expected, especially the parts between the trade-wind belts.
n.
A northern constellation near the pole. Its head, which is in the Milky Way, is marked by a triangle formed by three stars of the fourth magnitude. See Cassiopeia.
n.
A limicoline bird of Europe and Asia (Pavoncella, / Philommachus, pugnax) allied to the sandpipers. The males during the breeding season have a large ruff of erectile feathers, variable in their colors, on the neck, and yellowish naked tubercles on the face. They are polygamous, and are noted for their pugnacity in the breeding season. The female is called reeve, or rheeve.
n. pl.
A division of Lepidoptera, including the moths, and hawk moths, which have the antennae variable in form.
n.
A quantity which may increase or decrease; a quantity which admits of an infinite number of values in the same expression; a variable quantity; as, in the equation x2 - y2 = R2, x and y are variables.
n.
A constellation of the northern hemisphere, situated between Cepheus and Perseus; -- so called in honor of the wife of Cepheus, a fabulous king of Ethiopia.
n.
That which is variable; that which varies, or is subject to change.