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: 1302
correspondence
  هم‌پتوازی   
hampatvâzi

Fr.: correspondance   

The act, fact, or state of agreeing or conforming.

Verbal noun from → correspond.

correspondence principle
  پروز ِ همپتوازی   
parvaz-e hampatvâzi

Fr.: principe de correspondance   

The principle first put forward by N. Bohr according to which the behavior of quantum mechanical laws reduce to classical laws in the limit of large quantum numbers.

correspondence; → principle.

Corvus
  کلاغ   
Kalâq (#)

Fr.: Corbeau   

The Crow. A small but fairly conspicuous → constellation in the Southern Hemisphere lying south and west of → Virgo and east of → Crater.

L. corvus "raven," Gk. korax "raven," korone "crow," PIE base *qer-, *qor-, imitative of harsh sounds, cf. Pers. kalâq, Skt. kâkola- "raven."

Kalâq, Mid.Pers. warag, varâq "crow," Lori qelâ, Kordi qel, cf. Skt. kâkola- "raven," PIE base *qer-, *qor-, as above.

cosecant
  کوسکانت   
kosekânt (#)

Fr.: cosecante   

The → secant of the complement of an arc or angle; abbreviation csc. If θ is an → acute angle of a → right triangle, csc θ = → hypotenuse/(opposite side).

co-; → secante.

cosine
  کوسینوس   
kosinus (#)

Fr.: cosinus   

A trigonometric function giving the ratio of the side adjacent to a given angle to the hypotenuse.

Mod.L. complementi sinus, → com-; → sine.

cosmic
  کیهانی   
keyhâni (#)

Fr.: cosmique   

Of or relating to the → Universe (instead of universal which may lend to confusion), to the → outer space.

Adj. from → cosmos

cosmic acceleration
  شتاب ِ کیهانی   
šetâb-e keyhâni

Fr.: accélération cosmique   

accelerating Universe.

cosmic; → acceleration.

Cosmic Background Explorer (COBE)
  پویشگر ِ زمینه‌ی ِ کیهانی   
puyešgar-e zamin-ye keyhâni

Fr.: Satellite COBE   

NASA's satellite, designed to measure the diffuse infrared and → cosmic microwave background radiation from the early → Universe. It was launched on November 18, 1989 and carried three instruments: DIRBE (the Diffuse InfraRed Experiment), DMR (Differential Microwave Radiometers), and FIRAS (Far-InfraRed Absolute Spectrophotometer). The COBE observations showed that the cosmic microwave background spectrum matches that of a → blackbody of temperature 2.725 ± 0.002 K. COBE also found anisotropies in the cosmic microwave background at a level of a part in 100,000 (→ cosmic microwave background anisotropy). These tiny variations in the intensity of the CMB over the sky show how matter and energy was distributed when the Universe was still very young. Later, through a process still poorly understood, the early structures developed into galaxies, galaxy clusters, and the large scale structure that we see in the Universe today. Two of COBE's principal investigators, George Smoot and John Mather, received the Nobel Prize in Physics in 2006 for their work on the project.

cosmic; → background; → explorer.

cosmic background radiation
  تابش ِ پس‌زمینه‌ی ِ کیهانی   
tâbeš-e paszaminé-ye keyhâni

Fr.: rayonnement du fond cosmique   

cosmic microwave background radiation (CMBR).

cosmic; → background; → radiation.

Cosmic Dark Age
  عصر ِ تاریک ِ کیهانی   
asr-e târik-e keyhâni

Fr.: âge sombre cosmique   

The period of time in the early history of the Universe, between the → recombination era and the advent of the → first stars.

cosmic; → dark; → age.

cosmic defect
  آک ِ کیهانی   
âk-e keyhâni

Fr.: défaut cosmique   

Topological irregularities in the → space-time  → continuum, caused by the abrupt cooling of the → early Universe shortly after the → Big Bang, as predicted by some → cosmological models. These regions of immensely high density might have been the seeds of → structure formation through → gravity. Same as → topological defect.

cosmic; → defect.

cosmic distance scale
  مرپل ِ دورای ِ کیهانی   
marpel-e durâ-ye keyhâni

Fr.: échelle des distances cosmiques   

Measurement of the distances to the farthest objects in the Universe based on a bootstrapping series of methods, each applicable to more distant objects, and each dependent on the previous methods.

cosmic; → distance; → scale.

cosmic dust
  غبار ِ کیهانی، گرد ِ ~   
qobâr-e keyhâni (#), gard-e ~ (#)

Fr.: poussière cosmique   

Aggregations of matter on the order of a fraction of a micron across, irregularly shaped, and composed of → carbon and/or → silicates found in the → interstellar medium. Dust absorbs stellar light causing large dark patches in regions of the → Milky Way Galaxy and dark bands across other galaxies.

cosmic; → dust.

cosmic energy equation
  هموگش ِ کاروژ ِ کیهانی   
hamugeš-e kâruž-e keyhâni

Fr.: équation de l'énergie cosmique   

Same as the → Layzer-Irvine equation.

cosmic; → energy; → equation.

cosmic expansion
  گسترش ِ کیهانی   
gostareš-e keyhâni

Fr.: expansion cosmique   

Same as the → expansion of the Universe.

cosmic; → expansion.

cosmic Eyelash (SMM J2135-0102)
  مژه‌ی ِ کیهانی   
može-ye keyhâni

Fr.: Cil cosmique   

A galaxy at a → redshift of z = 2.3259 lying behind a massive → cluster of galaxies and magnified by the → lensing effect of the cluster. It was first discovered in → submillimeter waves. The lensing cluster lies at a redshift z > 1.5 causing an → amplification factor for the background galaxy of 32 (A. M. Swinbank et al. 2010, Nature 464, 733).

cosmic; eyelash, from → eye + lash, from M.E. lashe (n.) lashen (v.) "to blow, stroke." Such called because of its narrow and elongated shape.

Možé "eyelash," from Mid.Pers. mec "eyelash," mecitan "to blink;" cf. Skt. mes "to open the eyes;" O.C.S. po-mežiti "to close the eyes;" keyhâni, → cosmic.

cosmic filament
  رشته‌ی ِ کیهانی   
rešte-ye keyhâni

Fr.: filament cosmique   

A very large-scale structure made of → galaxy clusters threaded like beads on a chain. Cosmic filaments are chiefly made up of → dark matter but also, to a lesser extent, of → baryonic matter. They are the largest entities in the → Universe and can be up to 1 billion → light-years long. They are separated by great → voids.

cosmic; → filament.

cosmic horizon
  افق ِ کیهانی   
ofoq-e keyhâni (#)

Fr.: horizon cosmologique   

The → observable region of the → Universe, limited in extent by the distance → light has traveled during the time elapsed since the beginning of the Universe (→ Big Bang). No signal from the objects lying beyond the cosmic horizon can be received because light has not yet had enough time to travel the distance. The cosmic horizon can be defined in two ways:
1) The size of the → observable Universe as derived from ct, where c is the → speed of light and t is the → age of the Universe, 13.8 billion years, hence 13.8 billion → light-years.
2) The → comoving distance. The distance given above corresponds to the size Universe had 13.8 billion years ago. Since then the Universe has been growing at a rate of 3.52c. Therefore, the current radius of the observable Universe is about 48 × 109 light-years. Same as → particle horizon, → Hubble distance, → Hubble radius, and → Hubble length. See also → sound horizon.

cosmic; → horizon.

cosmic infrared background (CIB)
  پس‌زمینه‌ی ِ فروسرخ ِ کیهانی   
paszamine-ye forusorx-e keyhâni

Fr.: le cosmique infrarouge   

A diffuse radiation which consists of the cumulative infrared emission from all galaxies throughout cosmic history. It is about 50 times weaker than the → cosmic microwave background radiation (CMBR). Since the CIB is produced by the dust within such galaxies, it carries a wealth of information about the processes of star formation therein.

cosmic; → infrared; → background.

cosmic microwave background anisotropy
  ناهمسانگردیِ تابشِ ریزموجِ پس‌زمینه‌یِ کیهانی   
nâhamsângardi-ye tâbeš-e rizmowj-e paszaminé-ye keyhâni

Fr.: anisotropies du rayonnement du fond cosmique microonde   

Tiny fluctuations in the intensity of the → cosmic microwave background radiation (CMBR) as a function of angular position over the sky, first discovered in the → Cosmic Background Explorer (COBE) observations. At a level of 1 part in 100,000, these temperature variations trace the distribution of matter and energy when the Universe was very young, about 380,000 years old. Since the CMB spectrum is described to a high precision by a → blackbody law with temperature T0, it is usual to express the anisotropies in terms of temperature fluctuations ΔT/T0 and expand them on the sky in → spherical harmonic series ΔT/T0 (θ,φ) = Σ almYlm(θ,φ), where θ and φ are the → spherical polar coordinates, Ylm is the spherical harmonic functions with → multipole index l, and the sum runs over l = 1, 2, ..., ∞, m = -l, ..., l, giving 2l + 1 values of m for each l, and alm is the multipole moment of the decomposition. The power spectrum of the anisotropies is defined as Cl≡ mean | alm |2 = 1/(2l + 1) Σ mean | alm |2. See also → CMB angular power spectrum.

cosmic; → microwave; → background; → anisotropy.

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