An Etymological Dictionary of Astronomy and Astrophysics

فرهنگ ریشه شناختی اخترشناسی-اخترفیزیک

M. Heydari-Malayeri    -    Paris Observatory



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Number of Results: 1310
  اینسوماهی، اینسومانگی   
insumâhi, insumângi

Fr.: cislunaire   

Lying between the Earth and the orbit of the Lune. → translunar.

L. cis, cistra "on this side," cf. Gk. ekeinos "that person," E. he, it, O.H.G. he.

Insuumâhi, insumângi, from insu "this side," from in "this" + su "side" + mâhi, mângilunar, → moon.

šahr (#)

Fr.: ville, cité   

Any large town or populous place.

M.E. cite, from O.Fr. cite "town, city," from L. civitas "citizenry; community," from civis "native, townsman;" related to L. cuna "cradle; bed;" Gk. kome "village;" Skt. śiva- "auspicious, dear;" O.E. ham "dwelling, house, village;" E. home; Ger. Heim (→ hamlet); Iranian dialects kiye "house, home;" Xonsâri ki "house;" Anâraki xiya, Tâti Karingân , Sangesari keh "house, home;" PIE *kei- "to lie; bed."

Šahr "city," from Mid.Pers. šahr "land, country, city;" O.Pers. xša- "to rule," pati-xša- "to have lordship over," Xšyāršan- "hero among kings" or "ruling over heroes" the proper name of the Achaemenid emperor Helenized as Xerxes, upari.xšay- "to rule over," xšāyaθiya- "king;" Mid.Pers. šâh "king," pâdixšâ(y) "ruler; powerful; authoritative;" Mod.Pers. šâh "king," pâdšâh "protecting lord, emperor, monarch, king," šâyestan "to be worth, suit, fit;" Av. xšā(y)- "to rule, have power," xšayati "has power, rules," xšāyô "power;" cf. Skt. ksā- "to rule, have power," ksáyati "possesses;" Gk. ktaomai "I acquire," ktema "piece of property;" PIE base *tkeh- "to own, obtain."


Fr.: civil   

Of or relating to citizens and their interrelations with one another or with the state.

M.E., from L. civilis "of or proper to a citizen," from civis "citizen, townsman," from PIE *kei- "to lie, homestead;" → city.

Šârin, from šâr "city," variant šahr; Mid.Pers. šahr "city, country, land" (O.Pers./Av. xšaθra- "kingship, kingdom," (Skt. ksatra-), from xšay-, "to rule;" cf. Skt. ksayati "possesses;" Gk. ktaomai "I acquire," ktema "piece of property") + -in suffix of adjectives, relations and agent nouns (as in qamin "sorrowful," nušin "sweet, agreeable (thing)."

civil time
  زمان ِ شارین   
zamân-e šârin

Fr.: temps civil   

Mean solar time.

civil; → time.

civil twilight
  نیمتاب ِ شارین   
nimtâb-e šârin

Fr.: crépuscule civil   

The time between sunset or sunrise and the moment when the Sun's center lies 6° below the horizon. → astronomical twilight.

civil; → twilight.


Fr.: civilisation   

1) An advanced state of human society, in which a high level of culture, knowledge, production, and legal organization has been reached. The people or nations that have reached such a state.
2) The act or process of civilizing or being civilized.

verbal noun of → civilize.


Fr.: 1) civiliser; 2) se civiliser   

1) To cause to evolve out of a primitive state as to technical, moral, or intellectual matters.
2) To acquire the customs and manners of a civil community.

civil + → -ize.

  شارین‌مند، شارینیده   
šârinmand, šârinidé

Fr.: civilisé   

1) Of a society or country, having well-organized laws and rules about way of life.
2) Cultured, polite.

Past participle of → civilize.

  ۱) زویه؛ ۲) زوییدن   
1) zuyé 2) zuyidan

Fr.: 1) réclamation, revendication; 2) réclamer, revendiquer   

1a) A demand for something as due; an assertion of a right or an alleged right.
1b) An assertion of something as a fact.
2a) To demand by or as by virtue of a right; demand as a right or as due.
2b) To assert and demand the recognition of (
See also: → acclaim, → declaim, → proclaim.

M.E. claimen, from O.Fr. clamer "to call, name, describe; claim; complain," from L. clamare "to cry out, shout, proclaim," from PIE *kele- "to shout;" cf. Skt. usakala "cock," literally "dawn-calling;" Middle Irish cailech "cock;" Gk. kalein "to call;" L. calare "to announce solemnly;" O.H.G. halan "to call;" O.E. hlowan "to make a noise like a cow;" Lith. kalba "language."

Zuyidan, from zu- "to call;" cf. Av. zu- "to call;" O.Pers. (+ pati) zu- "to proclaim;" Sogd. 'zw- "to call;" Pashtu zwag "noise, clamour;" Skt. havi "to call upon, invoke;" O.C.S. zvati; Slov. zvati; Toch. B kwā- "to call out to, invite" (Cheung 2007).

Clapeyron equation
  هموگش ِ کلاپرون   
hamugeš-e Clapeyron

Fr.: équation de Clapeyron   

An equation that relates the temperature and pressure dependence of phases in equilibrium with the heat interaction and volume change associated with a phase change: dP/dT = L/T ΔV, where dP/dT is the slope of the coexistence curve, L is the → latent heat, T is the temperature, and ΔV is the volume change of the phase transition.

Named after Émile Clapeyron (1799-1864), a French engineer and physicist, one of the founders of → thermodynamics; → equation.

  آرونش، رونه‌کرد   
âruneš, runekard

Fr.: clarification   

The action of making a statement or situation less confused and more comprehensible.

Verbal noun of → clarify.

  آرونیدن، رونه کردن   
ârunidan, runé kardan

Fr.: clarifier   

1) To make (an idea, statement, etc.) clear or intelligible; to free from ambiguity.
2) To remove solid matter from (a liquid); to make into a clear or pellucid liquid (

clear; → -fy.

radé (#)

Fr.: classe   

General: A set, collection or group formed of members with certain attributes or traits in common.

From Fr. classe, from L. classis "summons, division of citizens for military draft, hence army, fleet, also class in general."

Radé "a line, series, row," from Mid.Pers. ratak "series, row," O.Pers. râd-, Av. raz- "to direct, put in line, set," Av. razan- "order."

Class 0
  رده‌ی ِ 0   
rade-ye 0

Fr.: Classe 0   

A low-mass → protostar deeply embedded in a → circumstellar dusty envelope and resulting from the → gravitational collapse of a dense → pre-stellar core. This stage in the process of star formation occurs typically a few 104 years after the onset of the collapse. Class 0 protostars represent the earliest stage of → young stellar objects. The → spectral energy distribution (SED) of a Class 0 object resembles a → blackbody spectrum at a temperature below ~ 15-30 K, peaking at → submillimeter wavelengths beyond 100 μm. The central protostar has not yet acquired its final mass, since → accretion is still going on, and the envelope (detected in submillimeter wavelengths) is more massive than the central protostellar mass. Moreover, these objects show powerful → bipolar ejections of material in the form of collimated → carbon monoxide (CO)outflows which distinguish them from the pre-stellar phase of star formation. The subsequent evolution of a Class 0 is a → Class I.

class; → zero.

Class I
  رده‌ی ِ I   
rade-ye I

Fr.: Classe I   

A protostellar phase resulting from the evolution of a → Class 0 object typically a few 105 years after the beginning of the → gravitational collapse. The protostar grows in mass due to → accretion from the envelope, which becomes less massive than the protostar. An → accretion disk forms around the protostar through which mass is transferred to the central object. The → spectral energy distribution (SED) changes with respect to that of a Class 0. The peak of the SED shifts to → far infrared wavelengths (below 100 μm) as the temperature of the dust rises. Emission from both the envelope (about 100 K) and the thick disk (a few 100 K) are observed. The SED has a positive → spectral index (αIR > 0), so that the bulk of the → luminosity (still due to accretion) emerges at the longer infrared wavelengths. Moreover, → bipolar outflows and → jets are observed which are generally less powerful than those in Class 0 objects. Class I objects evolve into → Class II.

class; → one.

Class II
  رده‌ی ِ II   
rade-ye II

Fr.: Classe II   

A stage in the evolution of low-mass → protostars resulting from a → Class I object about 106 years after the initial → gravitational collapse. Most of the envelope has been removed and the embedded object becomes visible at infrared and optical wavelengths. At this stage, the bulk of the material has → accreted onto the central object. A flattened → circumstellar disk or → protoplanetary disk is present in which material moves inward at a decreasing rate. The disk contributes only about 1% of the total mass of the system. Material from a remaining envelope may still accrete onto the outer parts of the disk. The → spectral energy distribution (SED) at → near infrared wavelengths is dominated by the emission of the central protostar and typically peaks around 2 μm, corresponding to temperatures around 1000 to 2000 K. At longer wavelengths an → infrared excess is observed, originating from the disk. The SED has a negative → spectral index (-1.5 < αIR < 0). Estimated disk masses and → accretion rates are 10-3 to 10-1 → solar masses and 10-8 solar masses per year, respectively. This stage initiates the → pre-main sequence stage of a star. The object is referred to as a → classical T Tauri star. The stellar → photosphere is revealed at optical wavelengths accompanied by strong → emission lines and photometric variability, but the infrared luminosity is far larger than can be explained by the photometric temperature and radius.

class; → two.

Class III
  رده‌ی ِ III   
rade-ye III

Fr.: Classe III   

An evolutionary stage in the formation of low-mass → protostars resulting from a → Class II object between 1 to 10 million years after the initial → gravitational collapse. At this stage → accretion has ceased completely and what remains from the → circumstellar disk is a → debris disk. The temperature and density of the → pre-main sequence star keep increasing as the object slowly contracts to its final size. Most of the → luminosity derives from protostellar contraction. The → spectral energy distribution (SED) resembles a stellar → blackbody, peaking at optical and infrared wavelengths. Minor → infrared excess is still observed. The SED has a negative → spectral index (αIR < -1.5). Class III objects are sometimes called → weak-line T Tauri stars.

class; → three.

kelâsik (#)

Fr.: classique   

1) Considered as the typical, traditional, or usual form of something. → classical T Tauri star.
2) → classical physics.

From classic (+ → -al), from Fr. classique, from L. classicus "belonging to a class, relating to the first or highest class of the Roman people," from classis perhaps akin to calare "to call."

Loan from Fr. classique, as above.

classical bulge
  کوژ ِ کلاسیک   
kuž-e kelâsik

Fr.: bulbe classique   

A → galaxy bulge that appears protruding from the disk plane when seen at an appropriate → inclination. Classical bulges are somewhat → spheroidal, featureless (no → spiral arms, → bars, → rings, etc.), contain mostly → old stars (not much dust or star-forming regions), and are kinematically hot, i.e. dynamically supported by the → velocity dispersion of their stars. Their → surface brightness profile follows the → de Vaucouleurs law. Currently, they are thought to form through → gravitational collapse or → mergers in violent events, inducing a fast → burst of star formation if gas is available. An example is the → Sombrero galaxy bulge (D. A. Gadotti, 2012, astro-ph/1208.2295).

classical; → bulge.

classical field theory
  نگره‌ی ِ کلاسیک ِ میدان   
negare-ye klâsik-e meydân

Fr.: théorie classique des champs   

The theory that studies distributions of → energy, → matter, and other physical quantities under circumstances where their discrete nature is unimportant. Classical field theory traditionally includes → Newtonian mechanics, Maxwell's → electromagnetic theory, and Einstein's theory of → general relativity. The main scope of classical field theory is to construct the mathematical description of → dynamical systems with an infinite number of degrees of freedom. The word "classical" is used in contrast to those field theories that incorporate → quantum mechanics (→ quantum field theory). Classical field theories are usually categorized as → non-relativistic and → relativistic.

classical; → field; → theory.

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