An Etymological Dictionary of Astronomy and Astrophysics
English-French-Persian

فرهنگ ریشه شناختی اخترشناسی-اخترفیزیک

M. Heydari-Malayeri    -    Paris Observatory

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Number of Results: 1244
conversion factor
  کروند ِ هاگرد   
karvand-e hâgard

Fr.: facteur de conversion   

1) A numerical factor that, by multiplication or division, translates one unit or value into another.
2) In → molecular cloud studies, a factor used to convert the → carbon monoxide (CO) line intensity to → molecular hydrogen (H2) → column density; usually denoted XCO = I(CO) / N(H2). This useful factor relates the observed CO intensity to the cloud mass. A general method to derive XCO is to compare the → virial mass and the 12CO (J = 1-0) luminosity of a cloud. The basic assumptions are that the CO and H2 clouds are co-extensive, and molecular clouds obey the → virial theorem. However, if the molecular cloud is subject to ultraviolet radiation, selective → photodissociation may take place, which will change the situation. Moreover, molecular clouds may not be in → virial equilibrium. To be in virial equilibrium molecular clouds must have enough mass, greater than about 105 solar masses. The way → metallicity affects XCO is a matter of debate, and there is no clear correlation between XCO and metallicity. Although lower metallicity brings about higher ultraviolet fields than in the solar vicinity, other factors appear to be as important as metallicity for the determination of XCO. In the case of the → Magellanic Clouds, XCO(SMC) = 14 ± 3 × 1020 cm-2 (K km s-1)-1, which is larger than XCO (LMC) = 7 ± 2 × 1020 cm-2 (K km s-1)-1. An independent method to derive XCO is to make use of the gamma ray emission from a cloud. The flow of → cosmic ray protons interacts with interstellar low-energy hydrogen nuclei in clouds creating neutral → pions. These pions quickly decay into two gamma rays. It is therefore possible to estimate the number of hydrogen nuclei and hence the cloud mass from the gamma ray counts. Such a gamma-ray based conversion factor is estimated to be 2.0 × 1020 cm-2 (K km s-1)-1 for Galactic clouds, in good agreement with the result obtained from the virial method. However, the gamma ray flux is not well known in general, so this method is uncertain as well. See, e.g., Fukui & Kawamura, 2010 (ARAA 48, 547).

conversion; → factor.

convert
  هاگرد کردن   
hâgard kardan

Fr.: convertir   

1) To change units of one measuring or calculating system into units of another.
2) To transform from one material or state to another.

M.E. converten, O.Fr. convertir, from L. convertere "to turn around, transform," from → com- "together" + vertere "to turn;" cognate with Mod.Pers. gardidan "to change, to turn," → conversion.

Compound verb from hâgard, → conversion, + kardan "to do, to make," → -ize.

converter
  هاگردگر   
hâgardgar

Fr.: convertisseur   

A device that receives data in one form and converts it to another. → analog-to-digital converter.

convert; → -er.

convex
  کوژ   
kuž (#)

Fr.: convexe   

Having a surface that is curved or rounded outward.

From M.Fr. convexe, from L. convexus "vaulted, arched," p.p. of convehere "to bring together," from → com- "together" + vehere "to bring" (cf. Skt. vah- "to carry, lead," vahitra "vehicle," Av. vazaiti "to lead," Mid.Pers. waz-, wazidan "to carry away," Gk. oxos "chariot," PIE base *wegh- "to go, carry, drive").

Kuž "humped," Mid.Pers. kôf "hill, mountain; hump" (Mod.Pers. kuh, "mountain"), kôfik "humpbacked," O.Pers. kaufa-, Av. kaofa- "mountain."

convex lens
  عدسی ِ کوژ   
adasi-ye kuž (#)

Fr.: lentille convexe   

A lens that converges an incident beam of light to a focus.

convex; → lens.

convocation
  هم-وچ، هموچ   
hamvac

Fr.: convocation   

The act of convoking. The state of being convoked.

Verbal noun of → convoke.

convoke
  هم-وچیدن، هموچیدن   
hamvacidan

Fr.: convoquer   

To call together; summon to meet or assemble (Dictionary.com).

M.E., from M.Fr. convoquer, from L. convocare "to call together," from → con- "together," + vocare "to call," from vox, → voice.

Hamvacidan, from ham-, → com-, + vac "word," → voice, + -idan infinitive suffix.

convolution
  هماگیش   
hamâgiš

Fr.: convolution   

1) A mathematical combination of two functions which involves multiplying the value of one function at a given point with the value of another function, the weighting function, for a displacement from that point and then integrating over all such displacements. The process is repeated for every point of the function. Convolution expresses how the shape of a function is altered by the other. In mathematical terms, the convolution of two functions f(x) and g(x) is defined by: f*g = ∫f(u)g(x - u) du, integral from -∞ to +∞.
2) Astro.: Convolution describes how an instrument, through its transfer function, affects an input signal. → deconvolution.

Verbal noun of → convolve.

convolution theorem
  فربین ِ هماگیش   
farbin-e hamâgiš

Fr.: théorème de convolution   

A theorem stating that the → Fourier transform of the convolution of f(x) and g(x) is equal to the product of the Fourier transform of f(x) and g(x): F{f*g} = F{f}.F{g}.

convolution; → theorem.

convolve
  هماگیشیدن   
hamâgišidan

Fr.: convoluer   

1) To roll or wind together.
2) To bring about a → convolution.

From L. convolvere "to roll together," from → com- "together" + volvere "to roll, turn," PIE base *wel- "to turn, revolve;" cf. Skt. valati "he turns," ulba- "womb, vulva," Gk. eilyein "to roll, wrap, fold."

Hamâgiš, from ham- "together", → com-, + âgišidan "to entwine, to twist" (Dehxodâ), from Mid.Pers. gyš- "to bind, tie," hangyš- "to fasten to;" cf. Sogd. patigyš- "to imprison, confine;" Proto-Ir. *kaš- "to imprison" (Cheung 2007).

cookie
  کوکی   
cookie

Fr.: cookie   

An identifier file that a website automatically places in the user's computer hard drive. The cookie is used by the website to identify that a user has been on the website previously. Users concerned about privacy may disable cookies in their browser's setting.

From Du. koekje "little cake," diminutive of koek "cake," from M.Du. koke, akin to cake, M.E., from O.N. kaka (O.H.G. kuocho "cake"), any relation with Pers. kâk "biscuit; dry bread"? (loaned in Ar. ka'k).

cool
  سرد   
sard (#)

Fr.: froid   

Moderately cold.

M.E., from O.E. col, PIE base *gel- "cold, to freeze."

Sard "cold, cool," from Mid.Pers. sart, Av. sarəta- "cold," Skt. śiśira- "cold," Ossetian sald "cold," L. calidus "warm," Lith. šaltas "cold," Welsh clyd "warm," PIE *keltos- "cool".

cool hypergiant
  هیپرغول ِ سرد   
hiperqul-e sard

Fr.: hypergéante froide   

A highly unstable, → very massive star lying just below the empirical upper luminosity boundary in the → H-R diagram (→ Humphreys-Davidson limit) with spectral types ranging from late A to M. Cool hypergiants very likely represent a very short-lived evolutionary stage, and are distinguished by their high → mass loss rates. Many of them also show photometric and spectroscopic variability, and some have large → infrared excesses and extensive circumstellar ejecta. The evolutionary state of most of these stars is not known but they are all → post-main-sequence stars (Humphreys, 2008, IAUS 250).

cool; → hypergiant.

coolant
  سردگر   
sardgar

Fr.: refroidissant   

An agent of → cooling process.

cooling.

cooling
  ۱) سردش؛ ۲) سردکننده، سردگر   
1) sardeš; 2) sardkonandé, sardgar

Fr.: 1) refroidissement; 2) refroidissant   

1) The process of losing heat; a falling temperature.
2) The participial adjective of to cool.

cool; → -ing.

cooling flow
  تچان ِ سردش   
tacân-e sardeš

Fr.: flot de refroidissement   

A phenomenon observed in a → cluster of galaxies, whereby the cluster core loses energy via X-ray radiation because of the collisions between the gas particles. The radiation rate is proportional to the square of the density, and the → cooling time, which remains in the outer parts too large, becomes smaller than the → Hubble time in the core. As a result, the central regions of clusters of galaxies cool down; and since in the center of a cluster gas pressure and gravitational attraction are in equilibrium, the gas density has to rise to maintain the pressure necessary for supporting the outer layers of gas. To cause its density to rise, the cooled gas has to flow inward. As the densest gas, which cools quickest, is already concentrated in the center of the cluster, the inward flow will start at the center, soon followed by the outer layers. This flow of gas is called the cooling flow. Cooling flows are moderated through feedback due to the → supermassive black hole in the nucleus of the central galaxy. The gas inflow to the center fuels the → active galactic nucleus (AGN). The latter then heats again the gas through its → radio jets.

cooling; → flow.

cooling line
  خط ِ سردکننده، ~ سردگر   
xatt-e sardkonandé, ~ sardgar

Fr.: raie de refroidissement   

The spectral → emission line through which the → colling process takes place.

cooling; → line.

cooling process
  فراروند ِ سردش   
farâravand-e sardeš

Fr.: processus de refroidissement   

The process of → radiative cooling in which the → temperature of an astrophysical system decreases due to the radiation of a major → emission line. For example, → molecular → emission at → millimeter wavelengths and → submillimeter wavelengths results in decreasing the temperature in molecular clouds. At temperatures less than 300 K, the main → coolant is the → carbon monoxide (CO) molecule which contains most of the carbon. Similarly, the → [C II] line is a major coolant in → photodissociation regions. See also → line cooling, → cooling time.

cooling; → process.

cooling time
  زمان ِ سردش   
zamân-e sardeš

Fr.: temps de refroidissement   

1) The time in which a → white dwarf cools to half its temperature. It depends on the composition, the mass, and the actual luminosity at some point in time. Cooling time is given by the relation: t = 8.8 × 106 (12/A) (M)5/7 (μ/2)-2/7 (L)-5/7 in years, where M and L are mass and luminosity in solar units, A the mean → atomic mass, and μ the → mean molecular weight (Iben & Tutukov, 1984, ApJ 282, 615). See also → Mestel theory; → white dwarf crystallization.
2) The time needed by a → plasma to radiate its thermal energy. The cooling time is directly proportional to the square root of the temperature and inversely proportional to the density. It turns out that for the → intercluster medium in a → cluster of galaxies this time is longer than the → age of the Universe. At the centers of some clusters, however, the cooling time is smaller than the age of the Universe due to the presence of a → cooling flow.

cooling; → time.

coordinate
  ۱) همارا؛ ۲) هم‌آراستن   
1) hamârâ (#); 2) hamârâstan

Fr.: 1) coordonnée; 2) coordonner   

1) Any of a series of numbers which, in relation to a given → frame of reference, locate a point in space. See also: → astronomical coordinatescanonical coordinatesCartesian coordinatescelestial coordinatescylindrical coordinatesequatorial coordinatesGalactic coordinatesgeneralized coordinatespolar coordinatesspherical coordinatesprecessed coordinatestopocentric coordinates.
2) To place in the same order or rank; to organize in a concordant operation.

From L. co- "together," → com- + orinatus, p.p. of ordinare "to put in order, arrange," from ordo "order."

Hamârâ, from ham- "together," → com- + ârâ stem of ârâstan "to arrange, to set in order, adorn," Mid.Pers. ârây-, ârâstan "to arrange, adorn," O.Pers. râs- "to be right, straight, true," râsta- "straight, true" (Mod.Pers. râst "straight, true"), râd- "to prepare," Av. râz- "to direct, put in line, set," Av. razan- "order," Gk. oregein "to stretch out," L. regere "to lead straight, guide, rule," p.p. rectus "right, straight," Skt. rji- "to make straight or right, arrange, decorate," PIE base *reg- "move in a straight line."

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