Find link

language: af: Afrikaans als: Alemannisch [Alemannic] am: አማርኛ [Amharic] an: aragonés [Aragonese] ar: العربية [Arabic] arz: مصرى [Egyptian Arabic] as: অসমীয়া [Assamese] ast: asturianu [Asturian] az: azərbaycanca [Azerbaijani] azb: تۆرکجه [Southern Azerbaijani] ba: башҡортса [Bashkir] bar: Boarisch [Bavarian] bat-smg: žemaitėška [Samogitian] be: беларуская [Belarusian] be-tarask: беларуская (тарашкевіца) [Belarusian (Taraškievica)] bg: български [Bulgarian] bn: বাংলা [Bengali] bpy: বিষ্ণুপ্রিয়া মণিপুরী [Bishnupriya Manipuri] br: brezhoneg [Breton] bs: bosanski [Bosnian] bug: ᨅᨔ ᨕᨘᨁᨗ [Buginese] ca: català [Catalan] ce: нохчийн [Chechen] ceb: Cebuano ckb: کوردیی ناوەندی [Kurdish (Sorani)] cs: čeština [Czech] cv: Чӑвашла [Chuvash] cy: Cymraeg [Welsh] da: dansk [Danish] de: Deutsch [German] el: Ελληνικά [Greek] en: English eo: Esperanto es: español [Spanish] et: eesti [Estonian] eu: euskara [Basque] fa: فارسی [Persian] fi: suomi [Finnish] fo: føroyskt [Faroese] fr: français [French] fy: Frysk [West Frisian] ga: Gaeilge [Irish] gd: Gàidhlig [Scottish Gaelic] gl: galego [Galician] gu: ગુજરાતી [Gujarati] he: עברית [Hebrew] hi: हिन्दी [Hindi] hr: hrvatski [Croatian] hsb: hornjoserbsce [Upper Sorbian] ht: Kreyòl ayisyen [Haitian] hu: magyar [Hungarian] hy: Հայերեն [Armenian] ia: interlingua [Interlingua] id: Bahasa Indonesia [Indonesian] io: Ido is: íslenska [Icelandic] it: italiano [Italian] ja: 日本語 [Japanese] jv: Basa Jawa [Javanese] ka: ქართული [Georgian] kk: қазақша [Kazakh] kn: ಕನ್ನಡ [Kannada] ko: 한국어 [Korean] ku: Kurdî [Kurdish (Kurmanji)] ky: Кыргызча [Kirghiz] la: Latina [Latin] lb: Lëtzebuergesch [Luxembourgish] li: Limburgs [Limburgish] lmo: lumbaart [Lombard] lt: lietuvių [Lithuanian] lv: latviešu [Latvian] map-bms: Basa Banyumasan [Banyumasan] mg: Malagasy min: Baso Minangkabau [Minangkabau] mk: македонски [Macedonian] ml: മലയാളം [Malayalam] mn: монгол [Mongolian] mr: मराठी [Marathi] mrj: кырык мары [Hill Mari] ms: Bahasa Melayu [Malay] my: မြန်မာဘာသာ [Burmese] mzn: مازِرونی [Mazandarani] nah: Nāhuatl [Nahuatl] nap: Napulitano [Neapolitan] nds: Plattdüütsch [Low Saxon] ne: नेपाली [Nepali] new: नेपाल भाषा [Newar] nl: Nederlands [Dutch] nn: norsk nynorsk [Norwegian (Nynorsk)] no: norsk bokmål [Norwegian (Bokmål)] oc: occitan [Occitan] or: ଓଡ଼ିଆ [Oriya] os: Ирон [Ossetian] pa: ਪੰਜਾਬੀ [Eastern Punjabi] pl: polski [Polish] pms: Piemontèis [Piedmontese] pnb: پنجابی [Western Punjabi] pt: português [Portuguese] qu: Runa Simi [Quechua] ro: română [Romanian] ru: русский [Russian] sa: संस्कृतम् [Sanskrit] sah: саха тыла [Sakha] scn: sicilianu [Sicilian] sco: Scots sh: srpskohrvatski / српскохрватски [Serbo-Croatian] si: සිංහල [Sinhalese] simple: Simple English sk: slovenčina [Slovak] sl: slovenščina [Slovenian] sq: shqip [Albanian] sr: српски / srpski [Serbian] su: Basa Sunda [Sundanese] sv: svenska [Swedish] sw: Kiswahili [Swahili] ta: தமிழ் [Tamil] te: తెలుగు [Telugu] tg: тоҷикӣ [Tajik] th: ไทย [Thai] tl: Tagalog tr: Türkçe [Turkish] tt: татарча/tatarça [Tatar] uk: українська [Ukrainian] ur: اردو [Urdu] uz: oʻzbekcha/ўзбекча [Uzbek] vec: vèneto [Venetian] vi: Tiếng Việt [Vietnamese] vo: Volapük wa: walon [Walloon] war: Winaray [Waray] yi: ייִדיש [Yiddish] yo: Yorùbá [Yoruba] zh: 中文 [Chinese] zh-min-nan: Bân-lâm-gú [Min Nan] zh-yue: 粵語 [Cantonese]

jump to random article

searching for type variable 243 found (255 total)

alternate case: Type variable

Algol variable (687 words) [view diff] no match in snippet view article find links to article

Algol variables or Algol-type binaries are a class of eclipsing binary stars that are similar to the prototype member of this class, β Persei (Beta Persei

RR Lyrae-type variable stars close to the galactic center from the VVV ESO public survey

magnitude +7.4 star designated HD 200775. It is located near the Mira-type variable star T Cephei, and near the bright magnitude +3.23 variable star Beta

S Virginis is a Mira-type variable star in the constellation Virgo. Located approximately 700 parsecs (2,300 ly) distant, it varies between magnitudes

excess, with one being particularly high. There is one candidate B-type variable star, of 9th magnitude. A 2020 study of the variable stars in the cluster

approximately 7,000 light years from Earth. It is classified as an Alpha Cygni type variable star and its brightness varies from magnitude +5.12 to +5.22 with a

located near the Galactic Center. This star is listed as an eclipsing type variable star with the eclipse due to the passage of the planet as noted in the

the constellation of Sagittarius. This star is listed as an eclipsing type variable star with the eclipse due to the passage of the planet as noted in the

although estimates range from 50 to 80 million. A total of fifteen B-type variable stars have been detected in the cluster with four Be stars. Five of

TX Camelopardalis (abbreviated TX Cam) is a Mira-type variable star in the constellation Camelopardalis. It is a classical long period variable star with

approximately 510 light years from Earth. It is classified as a Beta Cephei type variable star and its brightness varies by 0.02 magnitudes with a period of 50

RY Sagittarii is a yellow supergiant and an R Coronae Borealis type variable star in the constellation Sagittarius. Although it ostensibly has the spectrum

white-hued glow of an A-type star. It is classified as a Delta Scuti type variable star and its brightness varies by 0.02 magnitudes over periods of 0

U Orionis (abbreviated U Ori) is a Mira-type variable star in the constellation Orion. It is a classical long period variable star that has been well

R Andromedae (R And) is a Mira-type variable star in the constellation Andromeda. Its spectral class is type S because it shows absorption bands of zirconium

W Hydrae is a Mira-type variable star in the constellation Hydra. The star is nearly located within the Solar neighborhood, at 320 light years from the

variable star of the FU Orionis-type, and was the second FU Orionis-type variable to be discovered. The system is located at a distance of approximately

approximately 158 light years from Earth. Classified as a Delta Scuti type variable star, its brightness varies by 0.010 magnitudes over a period of 1.61

Located in the lower part of the instability strip, it is a Delta Scuti-type variable that ranges in brightness from magnitude 6.16 down to 6.19 with a period

RZ Piscium (or RZ Psc) is a UX Orionis type variable star 608 light-years (186 pc) away, in the constellation Pisces. Over the years, the star has been

ellipsoidal variable with a 1.53 day period. Star C forms an Algol-type variable system with the close binary, showing both primary eclipses (when star

work, Second Catalogue of Variable Stars. It is classified as a Mira type variable star and its brightness varies between magnitude +4.5 and +10.0 with

of decreated gas. It is classified as a suspected Gamma Cassiopeiae type variable star with a visual magnitude varying from +4.30 down to +4.39. EAS (1997)

SU Aurigae is a T Tauri-type variable star in the constellation Auriga. It is located about 500 light-years (150 parsecs) away in the Taurus-Auriga Star

support its dating to very roughly 12 billion years old. 18 RR Lyrae type variable stars have been found within. It bore the first discovery of a millisecond

R Leonis is a red giant Mira-type variable star located approximately 370 light years away in the constellation Leo. The apparent magnitude of R Leonis

blue-white hue of a B-type star. This is classified as a Beta Cephei type variable star with a primary period of 0.16961 days (4 hours 4 minutes), completing

magnitude. For this reason, the star has been ruled out as a Beta Cephei-type variable star. Frosty Drew Observatory & Sky Theatre — Chi Carinae Cousins, A

stars known as slowly pulsating B stars. It was one of the first mid-B type variable stars in the northern hemisphere to be studied. The star undergoes non-radial

Ba, Pa, component of the δ Ser system; quadruple star; Delta Scuti-type variable star γ Ser γ 41 142860 78072 15h 56m 26.99s +15° 39′ 53.0″ 5.20 3.62

variable star, in 1951. This star is classified as a Gamma Cassiopeiae-type variable and its brightness varies from magnitude +3.22 to +3.55. In most versions

Sculptoris is a B-type giant star. It is classified as an SX Arietis type variable star and its magnitude varies by less than a tenth of a magnitude. The

was given its variable star designation in 2006. It is a BY Draconis-type variable, randomly varying in brightness by 0.04 in magnitude over a period of

Aquarii is a symbiotic star believed to contain a white dwarf and a Mira-type variable in a binary system. The orbital period is approximately 44 years. The

variable star designation in 1999. It is classified as an Alpha Cygni type variable star and its brightness varies from magnitude 4.19m to 4.23m. Its companion

strength of its neutral helium lines. It is classified as an SX Arietis type variable star and its brightness varies from magnitude +4.38 to +4.43 with a

RZ Normae is an R Coronae Borealis type variable star in the constellation Norma. It has a baseline magnitude of 10.2, dropping down to dimmer than 16

RT Normae is an R Coronae Borealis type variable star in the constellation Norma. It has a baseline magnitude of 9.8, dropping down to 14.7 at its minima

stellar classification of M6/7pe. It is classified as a pulsating Mira type variable star and its visual brightness varies with an average amplitude of 4

mass of the Sun and 6.4 times the Sun's radius. It is a Beta Cephei type variable star with a brightness that periodically varies from magnitude +3.38

published that discovery in 1956. It is classified as a Beta Cephei type variable star and its brightness varies from magnitude +4.79 down to +4.84 with

closer with a radial velocity of −23 km/s. This is a pulsating Mira-type variable star with a brightness that varies from magnitude +4.4 down to +13.5

variable star, in 1974. It is classified as an Alpha2 Canum Venaticorum type variable and its brightness varies from visual magnitude +6.43 down to +6.48

15 Cancri is an α2 CVn-type variable star in the zodiac constellation of Cancer, located around 980 light years away. It has the variable star designation

flare in 1948. Today similar flare stars are classified as UV Ceti type variable stars (using the abbreviation UV) in variable star catalogs such as

Tseraskaya (L. Ceraski) in 1908. It was classified as a U Geminorum-type variable, or dwarf nova. Observation since 1926 showed that this variable undergoes

variable star, in 1960. It is classified as an Alpha2 Canum Venaticorum type variable star and the combined brightness of the system varies from magnitude

the star's brightness varies. It is classified as a semiregular late-type variable, and its magnitude varies between +5.89 and +7.07 with a period of approximately

stellar classification of B3 Ib. It has been classified as a Beta Cephei type variable star, but the supergiant spectral type and a period of over a day mean

transient periodicities. Mu Centauri is classified as a Gamma Cassiopeiae type variable star and its brightness varies from magnitude +2.92 to +3.49. This star

distance to Cas OB14 is 880 pc. It is classified as an Alpha Cygni type variable star and its brightness varies by a few hundredths of a magnitude. Periods

observed elements in the outer atmosphere. It is an α² Canum Venaticorum-type variable star, ranging in magnitude from 5.15 down to 5.22. These variations

stellar classification of G8 III. It is classified as a BY Draconis type variable star. This is a chromospherically-active star with a longitudinal magnetic

constellation of Hydra, about 2.7° to the east of Gamma Hydrae. It is a Mira-type variable that ranges in apparent visual magnitude from 3.5 down to 10.9 over

located on the lower instability strip and is classified as a Delta Scuti type variable star. The apparent magnitude of the star varies in the range 4.26−4

helium are weaker than expected. The star is an Alpha2 Canum Venaticorum-type variable, ranging in magnitude from 5.35 down to 5.43 with a rotationally-modulated

an age of about 200 million years. It is classified as a BY Draconis type variable star and its brightness varies by 0.08 magnitudes. In 1986, it became

have been confirmed as members: 333 of these are classical T Tauri-type variable stars showing a near infrared emission excess, while the remainder are

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 period

designation in 1999. Samus et al. (2017) classify it as a slowly pulsating B-type variable star (SPB), which ranges from magnitude 5.84 down to 5.87 with a

main sequence star. It is classified as an Alpha2 Canum Venaticorum type variable star and its brightness varies from magnitude +5.22 to +5.27 with a

magnitude 5.39 secondary, component B, is classified as a Gamma Cassiopeiae type variable star. Due to its variable nature, the brightness of the system varies

6 days. Chi Serpentis is classified as an Alpha2 Canum Venaticorum type variable star, and its magnitude varies by 0.03 with a period of 1.5948 days

approximately 423 light years from Earth. It is classified as a Delta Scuti type variable star and its brightness varies from magnitude +6.06 to +6.15 with periods

light-years from the Sun. Since a member of the system is a β Cephei-type variable star, the magnitude is not fixed but varies slightly between +4.70 and

21 Canum Venaticorum is classified as an Alpha2 Canum Venaticorum type variable star and its brightness varies by 0.04 magnitudes over a period of 18

making it readily visible to the naked eye. Denebola is a Delta Scuti type variable star, meaning its luminosity varies very slightly over a period of a

Canis Majoris, in 1970. In the past it was classified as a Beta Cephei type variable star with an apparent magnitude that was measured varying between +5

with 4.6 times the Sun's radius. It is classified as a Delta Scuti type variable star and its magnitude varies by 0.04 with a period of 0.1557 days.

variable star designation in 1973. Samus et al. (2017) classify it as a Be-type variable star that ranges from a peak visual magnitude of 5.13 down to 5.44 with

astronomer V. P. Tsesevich in 1954. It was determined to be a W UMa-type variable and was noted for being located in the region of the Pleiades open cluster

This is a variable star tentatively classified as a slow irregular-type variable with a brightness that varies between magnitude +4.89 and +4.94. Koen

discovered by J. E. Winzer in 1974. It is an Alpha2 Canum Venaticorum-type variable with a period of 1.160898 days (or 7.0980 days), ranging in magnitude

times the radius of the star. It is classified as a Gamma Cassiopeiae type variable star and its brightness varies from magnitude +3.4 to +3.97. The star

effective temperature of 7,685 K. It is an Alpha2 Canum Venaticorum-type variable with magnitude ranging from 4.62 down to 4.67 over a period of 14 days

listed in the General Catalogue of Variable Stars as a possible β Cephei-type variable. Its brightness varies with an amplitude of 0m.02 over a period of 0

associates determined this is a young, rapidly rotating BY Draconis-type variable. A decade of photometry was used to determine a rotation period of 1

indicating a rapidly-rotating A-type main-sequence star. It is a Delta Scuti type variable star, with a dominant pulsation period of 0.1881 days and an amplitude

Variable, is a star in the constellation Crux. A long period (Mira-type) variable, its apparent magnitude ranges from 6.6 to 9.8 over 530 days. Hence

main-sequence stars. The primary component, Gliese 282A, is a BY Draconis type variable star with a stellar classification of K2V. It has an effective temperature

light-years (900 parsecs) from the Earth. Rho Leonis is an Alpha Cygni-type variable star, showing 0.032 magnitude brightness variations with a period of

used. The i-DTEC engine uses a 2-Stage turbocharger from Wastegate Type & Variable Geometry Turbocharger (VGT) left/right. It enables strong power from

along the equator. Epsilon Apodis is classified as a Gamma Cassiopeiae type variable star and its brightness varies between magnitudes 4.99 and 5.04. In

long-period modulation, is a variation in period and amplitude in RR Lyrae type variable stars. Sergey Blazhko first reported its observation by Lidiya Tseraskaya

component A, is yellow-white hued F-type subgiant star and a Gamma Doradus type variable, pulsating by 0.12 magnitudes with a dominant period of 1.45 days. There

with a stellar classification of G2V. It is an RS Canum Venaticorum-type variable that is magnetically active and a bright X-ray source. Despite this

the range A8-F0 V. One of the pair is an active RS Canum Venaticorum type variable star, which is causing the net brightness to vary with a period that

Atkins and D. S. Hall included it on a list of RS Canum Venaticorum type variable systems and showed it has an infrared excess. S. Jakate and associates

peculiarity in the spectrum. It is classified as a Gamma Cassiopeiae type variable star and its brightness varies from magnitude +5.43 to +5.61. This is

period of 20.67 hours. R. B. Carr in 1969 proposed this to be an Algol-type variable with a minor tidal distortion of the components, plus a large, anomalous

maximum brightness. The prototype of these variables, RV Tauri is a RVb type variable which exhibits brightness variations between magnitudes +9.8 and +13

Clang handles the type / variable name ambiguity of C/C++ https://eli.thegreenplace.net/2012/07/05/how-clang-handles-the-type-variable-name-ambiguity-of-cc/

Evolutionary stage main sequence + black hole Spectral type O7V(n)((f)) Variable type variable Astrometry Proper motion (μ) RA: +1.722 mas/yr Dec.: +0.603 mas/yr Parallax

with the variable star catalog name V1428 Aquilae. It is a BY Draconis type variable star subject to flare events. In August 2018, a group of scientists

April 29, 2018. It was previously known as a dwarf nova. A U Geminorum-type variable star or dwarf nova is a type of cataclysmic variable star consisting

1086/126229, S2CID 121064818. Fitch, Walter S. (May 1955), "The Cluster-Type Variable VZ Cancri", Astrophysical Journal, 121: 690, Bibcode:1955ApJ...121.

51.492158; -0.024249 Public transit Mudchute Type Arts venue Seating type Variable Capacity 60-145 Opened 1997; 28 years ago (1997) Website space.org.uk

reported by R. Kippenhahn in 1955. Huth in 1958 classified it as a β Lyr-type variable. W. Strohmeier found a short period of 15.46 hours in 1959, although

magnitude 6.5. The brightest star is Alpha Sculptoris, an SX Arietis-type variable star with a spectral type B7IIIp and an apparent magnitude of 4.3. It

magnitude 1.3, and lies 353 light-years from Earth. It is a Beta Cephei-type variable star with a variation of less than 0.1 magnitudes. γ Crucis or Gacrux

TESS light curve of a BY Dra-type variable star V1297 Her

seen (typical). There is a background of rich vascularity. Lobular type: Variable degrees of differentiation of uniform, round to oval cells with granular

instead: add_one(x) { var result; /* inferred-type variable result */ var result2; /* inferred-type variable result #2 */ result = x + 1; result2 = x + 1

parameterized by adding a type variable inside angle brackets (< and >) following the class name. It makes possible the use of this type variable in class members

General Catalog of Variable Stars classifies V1331 Cygni as an "INST" type variable, meaning a T Tauri star which shows rapid light variations. Its visual

from Earth and are of magnitude 5.7 and 6.1. R Draconis is a red Mira-type variable star with a period of about 8 months. Its average minimum magnitude

to include appearance of comets and variable brightness of Cepheid-type variable stars. Old astronomical plates exposed from the 1880s through the early

its variable star designation in 1924. It is classified as an Orion type variable star and its brightness varies irregularly between magnitudes +5.78

Lyrae system components (about 1 M☉). The prototype of the β Lyrae type variable stars is β Lyrae, also called Sheliak. Its variability was discovered

magnitude +2.51 to +2.65. It has been classified as a γ Cassiopeiae type variable. The energy from this star is being radiated at an effective temperature

S2CID 18759600 Celis S., L. (October 1975), "Photoelectric photometry of late-type variable stars", Astronomy and Astrophysics Supplement Series, 22: 9–17, Bibcode:1975A&AS

a batch of 2,675 new variables. It is classified as an Alpha Cygni type variable and its brightness varies from magnitude +4.69 to +4.75 as measured

the few irregular dwarf galaxies in the Local group where RR Lyrae-type variable stars have been observed. Others include the Magellanic Clouds. In 1999

engine collection on display at the Rolls-Royce Heritage Trust in Derby. Type: Variable thrust liquid-propellant rocket engine Length: 78.5 in (199.4 cm) Diameter:

VizieR. Celis S., L. (October 1975), "Photoelectric photometry of late-type variable stars", Astronomy and Astrophysics Supplement Series, 22: 9–17, Bibcode:1975A&AS

stellar classification of A8 Vn. It is classified as a Delta Scuti type variable star and its brightness varies from magnitude +4.28 to +4.31 with a

\alpha _{i}} are called quantified and any occurrence of a quantified type variable in τ {\displaystyle \tau } is called bound and all unbound type variables

S2CID 18759600. Celis S., L. (October 1975), "Photoelectric photometry of late-type variable stars", Astronomy and Astrophysics Supplement Series, 22: 9–17, Bibcode:1975A&AS

"A Survey of the Spectra and Radial Velocities of the Less Regular M-Type Variable Stars", Astrophysical Journal, 96: 344, Bibcode:1942ApJ....96..344J

confirmed by A. W. Roberts in 1895. Roberts determined this to be an Algol-type variable with a period of 2.416 days. In his 1915 study of eclipsing binaries

respectively). The primary is classified as an Alpha2 Canum Venaticorum-type variable star and the brightness of the system varies from magnitude +4.45 to

2018-06-18. Celis S., L. (October 1975), "Photoelectric photometry of late-type variable stars", Astronomy and Astrophysics Supplement Series, 22: 9–17, Bibcode:1975A&AS

close spectroscopic binary. Omicron Andromedae is a Gamma Cassiopeiae type variable star and the system's brightness varies from magnitude +3.58 to +3.78

of such a star, so similar flare stars are now classified as UV Ceti type variable stars. This star goes through fairly extreme changes of brightness:

ellipsoidal shape of that object, the system is also an RS Canum Venaticorum-type variable star. It is a magnetically active star with a brightness that varies

about a tenth of a magnitude. It is thought likely to be an α Cygni-type variable. van Leeuwen, F. (November 2007), "Validation of the new Hipparcos reduction"

temperature of 11,145 K. This is classified as a Gamma Cassiopeiae type variable star and its brightness varies from magnitude +4.68 down to +4.89. It

Chi1 and Chi2 mark the end of the club. Just east of Chi1 is the Mira-type variable red giant U Orionis. West from Bellatrix lie six stars all designated

abundance of silicon. The primary is classified an Alpha2 Canum Venaticorum type variable star and has a surface magnetic field of about 1 kG. Its projected rotational

into an ordinary B-type star. It is classified as a Gamma Cassiopeiae type variable star and its brightness varies from magnitude +4.45 to +4.71; a range

variable showing total eclipses of the brighter component, an Algol-type variable. In between the primary eclipses, there are slight brightness variations

is referred to as WX Ursae Majoris. It is characterized as a UV Ceti-type variable star that displays infrequent increases in luminosity. This star was

final stages of its life. The star is classified as an Alpha Cygni-type variable star and its brightness varies from magnitude +2.38 to +2.48 over a

.....0W. Hill, G.; Fisher, W. A. (January 1987). "Studies of early-type variable stars. IV. The orbit and physical dimensions for V373 Cas". Astronomy

American astronomer Olin J. Eggen. It was determined to be a Delta Scuti-type variable star, making it one of the first stars of that type to be identified

Cephei (S Cep), also designated as HD 206362, is a carbon star and Mira-type variable in the constellation Cepheus. Based on the measurement of its annual

Schwarzenberg-Czerny, A. (2013). "Time-resolved multicolour photometry of bright B-type variable stars in Scorpius". Astronomy & Astrophysics. 557: A1. arXiv:1307.2733

blue-white hue of a B-type star. This star is classified as an Alpha Cygni-type variable star that undergoes periodic non-radial pulsations, which cause its

a suspected variable star. S Piscis Austrini is a long-period Mira-type variable red giant which ranges between magnitude 8.0 and 14.5 over a period

A type variable star in the constellation Phoenix

Such a length function may be parametric polymorphic by including a type variable in its type signature, since the number of elements in the list is independent

Hemisphere, Omega Canis Majoris is classified as a Gamma Cassiopeiae-type variable star. Both the luminosity and the radial velocity vary with a primary

a stellar classification of A7V. It is classified as a Delta Scuti-type variable star and its brightness varies from magnitude +4.73 to +4.78 with a

nearly pole-on. This star is classified as an α2 Canum Venaticorum type variable star and its brightness varies by 0.03 magnitudes. It has 2.44 times

detected in 1992 by Edward J. Kennelly and colleagues. It is a Delta Scuti-type variable star with a period of 6.96753 h that varies from magnitude +3.02 down

the mass and much fainter. κ2 Boötis is classified as a Delta Scuti type variable star with a period of 1.08 hours Its brightness varies from magnitude

S2CID 18759600 Celis S., L. (October 1975), "Photoelectric photometry of late-type variable stars", Astronomy and Astrophysics Supplement Series, 22: 9–17, Bibcode:1975A&AS

from the TESS satellite found it to be an Alpha2 Canum Venaticorum-type variable star, consistent with its magnetic and chemical properties. The variability

RR Lyrae-type variable stars (not RR Lyr itself) close to the galactic center from the VVV ESO public survey

is an outlying component of the galaxy, and contains many RR Lyrae-type variable stars. It has a magnitude of 11.59 and is thought to be over 12 billion

YF120 YF120 at the National Museum of the U.S. Air Force Type Variable-cycle turbofan National origin United States Manufacturer General Electric First

109729 61532 12h 36m 23.47s +59° 29′ 13.0″ 8.11 −3.19 5930 M4IIIe Mira-type variable star HD 95127 95127 53733 10h 59m 35.0s +43° 48′ 52″ 8.15 0.77 978 K0

modes now modeled. Delta Scuti is the prototype of the Delta Scuti type variable stars. It is a high-amplitude δ Scuti type pulsator with light variations

of the Sun's radius. This star is suspected of being a BY Draconis-type variable star with the provisional variable star designation NSV 15017. It is

S2CID 119231169. Maxted, P. F. L.; et al. (September 1995), "Studies of early-type variable stars. XIV. Spectroscopic orbit and absolute parameters of HU Tauri"

Go (2013) A declaration binds a non-blank identifier to a constant, type, variable, function, label, or package. [...] The scope of a declared identifier

The revised version specifies a recursive function on types. (The type variable ϕ {\displaystyle \phi } is used to suggest a function rather than a

version was released as Bahnschrift, as Microsoft's first ever Open Type variable font. The Bahnschrift source was completely rebuilt from the ground

mean apparent magnitude of +3.40. It is classified as a Delta Scuti type variable star and its brightness varies from magnitude +3.35 to +3.42 with a

2011 (2011) Owner(s) Grant Achatz Nick Kokonas Head chef Grant Achatz Food type Variable Rating (Michelin Guide) Street address 953 W. Fulton Market City Chicago

Indonesia Traits Weight Male: 2–3 kg Female: 1–2 kg Egg color White to light brown Comb type Variable Classification Chicken Gallus gallus domesticus

General Catalogue of Variable Stars as V1298 Aquilae. It is a UV Ceti-type variable star and is known to be subject to frequent flare events. Its dynamics

University of Chicago in 1946 with a dissertation on the spectra of A-type variable stars. As a graduate student, he was an instructor at Yerkes Observatory

"Test";; - : string = "Test Test Test Test" The function twice uses a type variable 'a to indicate that it can be applied to any function f mapping from

either a spectroscopic binary or (more likely) a pulsating Gamma Doradus-type variable. Alchiba has 34% more mass and is 42% larger than the Sun. It is 4.3

G7III U−B color index +1.00 B−V color index +1.15 Variable type Unknown-type variable (B) Astrometry Radial velocity (Rv) −36.24±0.18 km/s Proper motion (μ)

and magnitude 5.9 that is 990 light-years from Earth. R And is a Mira-type variable star with a period of 409 days. Its maximum magnitude is 5.8 and its

In 1976, it was identified as a candidate SU Ursae Majoris (SU UMa)-type variable. It was found to be a double eclipsing binary system by Nikolaus Vogt

−17° 41′ 08.0″ Apparent magnitude (V) 10.90 - 21 Characteristics Spectral type variable Apparent magnitude (J) 11.555 ± 0.022 U−B color index +0.27 B−V color

Pashchenko, M. I.; Rudnitskii, G. M. (May 1999), "Observations of late-type variable stars in the water-vapor radio line. The supergiant VX Sagittarii",

Visualisation of Mira type variable

not be taken into account my_frame.f_type.random_mode(0); // the f_type variable will not be randomized for this frame instance. my_frame.randomize();

S2CID 18759600. Celis S., L. (October 1975), "Photoelectric photometry of late-type variable stars", Astronomy and Astrophysics Supplement Series, 22: 9–17, Bibcode:1975A&AS

Time lapse of the Cepheid type variable star Polaris illustrating the visual appearance of its cycle of brightness changes.

14595 11035 02h 22m 06.62s +22° 52′ 24.9″ 6.71 0.50 615 G3III Algol type variable, Vmax = 6.30m, Vmin = 7.10m, P = 153 d VY Ari VY 17433 13118 02h 48m

Ueno, Yuji (2014). "VLBI astrometry of AGB variables with VERA: A Mira-type variable T Lepus". Publications of the Astronomical Society of Japan. 66 (6):

S2CID 18759600. Celis, L. (October 1975), "Photoelectric photometry of late-type variable stars", Astronomy and Astrophysics Supplement Series, 22: 9–17, Bibcode:1975A&AS

Aries has its share of variable stars, including R and U Arietis, Mira-type variable stars, and T Arietis, a semi-regular variable star. R Arietis is a Mira

1086/324228. Rodriguez, E.; Zerbi, F. M. (1995). "A long period early F-type variable: HR8799". Information Bulletin on Variable Stars. 4170: 1. Bibcode:1995IBVS

than 5,000 years. The brighter component, γ2 Arietis, is an α2 CVn type variable star, a type of star with a strong magnetic field and enhanced spectral

Wrapper classes can be used to store the same value as of a primitive type variable but the instances/objects of wrapper classes themselves are Non-Primitive

identifier x character (len = 100) :: student_name ! declaring a character type variable with len 100 F does not have intrinsic support for object-oriented programming

by reference (alias) to a function, the object where the reference-type variable points to can also be changed, in addition to the object itself (if

.36S. Maxted, P. F. L.; et al. (September 1995), "Studies of early-type variable stars. XIII. Spectroscopic orbit and absolute parameters of TX Ursae

describes the type which results from replacing all occurrences of the type variable α (resp. term variable x) in τ {\displaystyle \tau } by the type σ (resp

Chris Dodd and Vadim Maslov. Bendersky, Eli. "How Clang handles the type / variable name ambiguity of C/C++". http://www.cs.berkeley

surface gravity of the Sun. Lalande 21185 is listed as a BY Draconis type variable star in the General Catalogue of Variable Stars. It is identified by

operation. The syntax for typecasting is as follows: (typecast_data_type) variable ..." Gopal, Arpita (2009). Magnifying C. PHI Learning Private Limited

1,937 M☉, of which about 24% is interstellar matter. A Delta Cephei type variable star designated U Sagittarii is a member of this cluster, as are two

diameter around 80 times that of the Sun. Classified as an Alpha Cygni type variable star, Aludra varies in brightness from magnitude 2.38 to 2.48 over a

brightening to 12.7 in outburst. SZ Crateris is a magnitude 8.5 BY Draconis type variable star. It is a nearby star system located about 42.9 ± 1.0 light-years

Var B may refer to: B-type variable star Variable declaration of "b" in computer programming M33 Var B, see List of most luminous stars This disambiguation

of the form eta :: F a -> G a, where a is a universally quantified type variable – eta knows nothing about the type which inhabits a. The naturality

(2000). "Serendipitous discovery of an irregular and a semi-regular type variable in the field of BY Draconis". Astronomy and Astrophysics. 364: 706.

maximum of 7.44 over a period of 5.0 days. Two of the brighter Mira-type variable stars in the constellation are R and S Boötis. Both are red giants that

keyword to a primitive type variable causes the variable to become immutable. However, applying final to a reference type variable only prevents that another

any direction. Unlike the 18-pounder, the 25-pounder used howitzer-type variable-charge ammunition. The 25-pounder was separate-loading; the shell was

constant array that doesn't even need an explicit declaration of a LABEL type variable: /* This implements the equivalent of */ /* the computed goto */ declare

MaybeProd a into a functor, the functoriality is only in the second type variable fmap g Nothing = Nothing fmap g (Just (x,y)) = Just (x, g y) The initial

either a spectroscopic binary or (more likely) a pulsating Gamma Doradus-type variable. If the latter is the case, it is estimated to be 1.39 times as massive

system in the constellation Leo Minor. It is an AM Canum Venaticorum-type variable star, a type of binary systems with ultra-short periods (between 5 and

AL-41F Type Variable cycle turbofan National origin Russia Manufacturer NPO Saturn Major applications Mikoyan Project 1.44 Developed from Saturn AL-31

by Hisense as of 2009. Huzhou production base is a Hisense inverter-type/variable-frequency air-conditioner production base is in Huzhou, Zhejiang, and

Draconis variable star designated as V1803 Cyg while 61 Cygni B is a flare type variable star named HD 201092 with their magnitudes varying 5.21 V and 6.03,

on the speed and torque level of the machine, as well as the motor type. Variable-frequency drives use pulse-width modulation, which introduces additional

of elements, where the type of elements is arbitrary (denoted by the type variable a), is either the empty list “[]” or the non-empty list “x:xs” consisting

interceptor, with an Atar 09B turbojet engine, featuring an eyelid type variable exhaust.[citation needed] The Mirage IIIC was armed with twin 30 mm

similar diameter and slightly lighter, driving Hamilton Standard bracket-type variable-pitch propellers. There was no guaranteed supply of the Twin Wasp and

Crosman Pumpmaster 760, Crosman 760 Pumpmaster Type (Variable) Multi-Pump Pneumatic Air Rifle Place of origin United States Production history Designer

the other setting stars. Pleione is classified as a Gamma Cassiopeiae type variable star, with brightness fluctuations that range between a 4.8 and 5.5

Astafan Type Variable-pitch turbofan National origin France Manufacturer Turbomeca First run 1969: 553  Developed from Turbomeca Astazou

and the type [Char] of the second argument ['x']. The polymorphic type variable a will be unified with Bool and the second argument [a] will be unified

148206 80488 16h 25m 47.70s +18° 53′ 33.0″ 6.70 −2.23 1989 M7III Mira-type variable HD 154345 154345 83389 17h 02m 36.40s +47° 04′ 54.8″ 6.74 5.46 59 G8V

and hydrogen. Its spectral type is G5V:e. SS Aurigae is an SS Cygni-type variable star, classified as an explosive dwarf. Discovered by Emil Silbernagel

procedure as shown below. PROCEDURE <Procedure ID/Name>(<Data Type> <Variable>,<Data Type> <Variable>...) Haggis Commands END PROCEDURE Haggis includes all the

tau function in number theory shear stress in continuum mechanics a type variable in type theories, such as the simply typed lambda calculus path tortuosity

outputvariable="$westCoastOnly"/> The sort statement sorts the content of a document-type variable or variable fragment based on key expressions and places the result

symbol (1 byte length, typically 4) 30 P-type, variable length packed decimal (1 byte length) 34 Z-type, variable length zoned decimal (1 byte length) 38

central region of Taurus, an equatorial constellation. This is a T Tauri-type variable star that ranges in apparent visual magnitude from 10.59 down to 10

Characteristics Evolutionary stage Luminous blue variable Spectral type variable (LBV) + O (WR?) Apparent magnitude (U) 6.37 Apparent magnitude (B) 6

take the form of a function call. In that case an initialized Person type variable can be thought of as the return value: int main() { Person r = Person("Wales"

over shocks; stabilizer bar; fully adjustable camber and toe Steering type variable-ratio rack-and-pinion Steering ratio 16.1:1 Turning circle 37.7 ft (1

which is comparable to the typical field strength of RS CVn or FK Com type variable stars. This is an evolving subgiant star with a very slow rotation period

wildcard can be either a class type, interface type, array type, or type variable. Upper bounds are expressed using the extends keyword and lower bounds

a young star about 400 light years from the Earth. It is a T Tauri-type variable star, ranging in brightness from magnitude 10.5 to 14.9 (in blue light)

type in the first letter if lowercase and the uppercase letters from a type/variable name then press Ctrl+space to be offered all the choices that match

making it almost twice the size of the Sun. It may be a Delta Scuti type variable star due to its variations in brightness; about 10 times a day the star's

capture#1 by method invocation conversion) where capture#1 is a fresh type-variable: capture#1 extends Animal from capture of ? extends Animal Since both

the AN/PVS-4 ceased entirely by 2002. The AN/PVS-4 uses a 25mm screw-type variable-gain Image Intensifier tube. Operational voltage is 3.0 Volts. Early

Japanese pitch-accent types   Keihan type (downstep plus tone)   Tokyo type (variable downstep)   N-kei (1-3 pattern) type (fixed downstep)   No accent   intermediate

class(parameters) variable = Nil Eiffel create variable or create «{TYPE}» variable.make_foo «(parameters)» or variable := create {TYPE} or variable :=

where the domain of answers is polymorphic, i.e., is implemented with a type variable. This continuation-passing implementation is mapped back to direct style

in 1988 with observations of SiO maser emission at 86 GHz from Mira-type variable stars. In 1993 its surface accuracy was reported to be 120 microns RMS

These variable stars discovered by Leland and Bailey are named cluster-type variable stars. They had a good working relationship and influenced each other

variable-section double cylindrical pier, the approach pier is snow lotus type variable-section round-end shaped pier, and the main span is a double-layered

subtractor proceeds as described under c). This was solved. In this last type variable basic keys are also used. Substituted cross addition. The indicator

S2CID 118651473. Hill, G.; Holmgren, D. E. (May 1995). "Studies of early-type variable stars. IX. Y Cygni". Astronomy and Astrophysics. 297: 127–134. Bibcode:1995A&A

; Garrido, R.; Saez, M. (13 April 1979). "HR 5343 A New Delta Scuti Type Variable". Information Bulletin on Variable Stars (1584). Bibcode:1979IBVS.1584

Characteristics Evolutionary stage T Tauri star Spectral type M0±2 Variable type variable nebula Astrometry Radial velocity (Rv) 20.3±3.5 km/s Distance 146.4±0

Jerzykiewicz, Mikolaj (October 1972). "HR 6684: A New Beta Cephei Type Variable Star". Publications of the Astronomical Society of the Pacific. 84 (501):

Characteristics Evolutionary stage T Tauri star Spectral type M1 ±2 Variable type variable nebula Astrometry Radial velocity (Rv) 7.4 km/s Distance 424 ly (130 pc)

S2CID 125853869. Hill, G.; Batten, A. H. (December 1984). "Studies of early-type variable stars. III. The orbit and physical dimensions for V380 Cygni". Astronomy

Andronov, I. L. (1998), Dusek, J. (ed.), "Cycle-to-Cycle Changes of Mira-type Variable X Oph", Proceedings of the 20th Stellar Conference of the Czech and