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: 1223
core elliptical galaxy
  کهکشان ِ بیضی‌گون ِ مغزه‌دار   
kahkešân-e beyzigun-e maqzedâr

Fr.: galaxie elliptique à coeur   

An → elliptical galaxy that displays a → surface brightness profile with a distinct break from a steep outer slope to a shallower inner → cusp. Core profiles mainly occur in very luminous elliptical galaxies and are considered the result of dissipation-less → mergers of two galaxies that have central → supermassive black holes (S. P. Rusli et al., 2013, AJ 146, 160).

core; → elliptical; → galaxy.

core mass function (CMF)
  کریای ِ جرم ِ مغزه   
karyâ-ye jerm-e maqzé

Fr.: fonction de masse des cœurs   

The mass distribution of → pre-stellar cores in → star-forming regions. The CMF is usually represented by dN/dM = Mα, where dM is the mass interval, dN the number of cores in that interval, and α takes different values in different mass ranges. In the case of → low-mass stars, it is found that the CMF resembles the → Salpeter function, although deriving the masses and radii of pre-stellar cores is not straightforward. The observational similarity between the CMF and the → initial mass function (IMF) was first put forth by Motte et al. (1988, A&A, 336, 150), and since then many other samples of dense cores have been presented in this context. For example, Nutter & Ward-Thompson (2007, MNRAS 374, 1413), using SCUBA archive data of the Orion star-forming regions, showed that the CMF can be fitted to a three-part → power law consistent with the form of the stellar IMF. Recent results, obtained using observations by the → Herschel Satellite, confirm the similarity between the CMF and IMF with better statistics (Könyves et al. 2010, A&A, 518, L106; André et al. 2010, A&A, 518, L102). Moreover, these works show that the CMF has a → lognormal distribution (i.e. dN/dlog M follows a → Gaussian form against log M), as is the case for the IMF at low masses (below about 1 solar mass).

core; → mass; → function.

core overshooting
  فرازد ِ مغزه   
farâzad-e maqzé

Fr.: dépassement du cœur   

convective overshooting.

core; → overshooting.

core profile
  فراپال ِ مغزه   
farâpâl-e maqzé

Fr.: profil de cœur   

A → profile representing the number density of stars in the → core of a galaxy.

core; → profile.

core-collapse supernova
  اَبَر-نو‌اختر ِ رمبش ِ مغزه   
abar-now-axtar-e rombeš-e maqzé

Fr.: supernova à effondrement de coeur   

A supernova arising from the → core collapse of a → massive star. Same as → Type Ib, → Type Ic, or → Type II supernova.

core; → collapse; → supernova.

core-dominated quasar
  کو‌آسار ِ مغزه چیره   
kuâsâr-e maqzé ciré

Fr.: quasar dont l'émission de cœur domine   

A → radio-loud quasar in which the central source is enhanced by → relativistic beaming and characterized by a → flat  → spectrum. It has been conjectured that this phenomenon is an → orientation effect. If a radio-loud quasar is seen along its → jet, it will appear as a core-dominated source. See also → lobe-dominated quasar.

core; → dominate; → quasar.

core-halo galaxy
  کهکشان ِ مغزه-هاله   
kahkešân-e maqzé-hâlé

Fr.: galaxie cœur-halo   

A radio galaxy characterized by an emission "halo" surrounding a more intense "core". About 20% of the known extended radio sources are of the core-halo type.

core; → halo; → galaxy.

coreshine
  مغزه‌تاب   
maqze-tâb

Fr.: éclat de cœur   

The → mid-infrared radiation which is scattered by unusually large → dust grains in the denser core regions of → molecular clouds. It occurs between 3 and 5 μm, when the light from nearby stars undergoes → scattering by the grains provided that they are about 1 μm in size, instead of 0.1 μm, as previously thought. Coreshine, which was detected in Spitzer IRAC data, is a widespread astronomical phenomenon. It is found across dozens of → dark clouds in the Galaxy and during all the phases of the → low-mass star formation (Pagani et al. 2010, Science, 329, 1622). See also → cloudshine.

core; → shine.

Coriolis acceleration
  شتاب ِ کوریولیس   
šetâb-e Coriolis (#)

Fr.: accélération de Coriolis   

The apparent acceleration corresponding to the → Coriolis force. It is the acceleration which, when added to the acceleration of an object relative to a rotating → reference frame and to its → centrifugal acceleration, gives the acceleration of the object relative to a fixed reference frame. Coriolis acceleration equals 2ω x v, where ω is the → angular velocity of the rotating reference frame and v is the radial velocity of a particle relative to the center of the rotating reference frame.

Coriolis effect; → force.

Coriolis effect
  اسکر ِ کوریولیس   
oskar-e Koriolis

Fr.: effet Coriolis   

The apparent → deflection of a body in motion with respect to the Earth, as seen by an → observer on the Earth, caused by the → Earth's rotation. Thus, a projectile fired due north from any point on the northern hemisphere will land slightly east of its target (deflection to the right). This involves two factors: 1) the eastward velocity of Earth's surface decreases from the → equator to the → poles, and 2) when an object starts to move north or south without being firmly connected to the ground it maintains its initial eastward speed (conservation of → angular momentum). Hence, an object travelling away from the equator will be heading east faster than the ground and will seem to be forced east. On the other hand, a ball fired in the northern hemisphere toward the equator deflects to the west. As for the southern hemisphere, a ball fired southward will deflect East. The projectile is not subject to this effect only on the equator, when it is thrown in an east-west direction. The Coriolis effect is therefore greater at higher → latitudes and smaller near the equator. This effect is of paramount importance to the large-scale → atmospheric circulation, the development of storms, and the sea-breeze circulation. In low pressure systems, i.e. zones where air ascends, the air is less dense than its surroundings and this creates a center of low atmospheric pressure. Winds blow from areas of high pressure to areas of low pressure, and so the surface winds would tend to blow toward a low pressure center. But, because of the Coriolis effect, they are deflected. In the northern hemisphere they are deflected toward the right, and fail to arrive at the low pressure center, but instead circulate around it → counterclockwise. In the southern hemisphere the circulation around a low pressure center would be → clockwise. Regarding high pressure systems in the northern hemisphere, a general clockwise rotation is created around the center. Same as the → Coriolis force. See also → geostrophic wind, → geostrophic flow.

Named after Gaspard Gustave Coriolis (1792-1843), French engineer and mathematician who first described this effect; → effect.

Coriolis force
  نیروی ِ کوریولیس   
niru-ye Coriolis (#)

Fr.: force de Coriolis   

An apparent, rather than real, force exerted on a body when it moves in a rotating → reference frame. Same as the → Coriolis effect.

Coriolis effect; → force.

Coriolis frequency
  بسامد ِ کوریولیس   
basâmad-e Coriolis

Fr.: fréquence de Coriolis   

A quantity defined as f = 2ω.sinθ, where ω is the Earth's → angular velocity, 2π/T, T is the rotation period of the Earth (→ sidereal day), and θ is the → latitude. Also called the → Coriolis parameter. This frequency occurs often in oceanographic studies. If an → iceberg is floating in a frictionless sea, and is given a push and allowed to move freely, it will travel in a circle of radius U/f, where U is the initial speed imparted by the push. This circle is called an inertial circle.

Coriolis effect; → frequency.

Coriolis theorem
  فربین ِ کوریولیس   
farbin-e Coriolis

Fr.: théorème de Coriolis   

The → absolute acceleration of a point P, which is moving with respect to a local → reference frame that is also in motion, is equal to the vector sum of:
a) the acceleration P would have if it were fixed to the moving system;
b) the acceleration of P with respect to the local moving system; and
c) a compound supplementary → Coriolis acceleration.

Coriolis effect; → theorem.

Cornu prism
  منشور ِ کورنو   
manšur-s Cornu (#)

Fr.: prisme de Cornu   

A combination of two 30° prisms, one of left-handed quartz and the other of right-handed quartz. The prisms are cemented together in order to get a 60° prism. The device will correct for light rotation and will transmit the beam in a straight direction. The Cornu prism has good ultraviolet transmitting qualities and no → double refraction.

Cornu's spiral; → prism.

Cornu's spiral
  مارپیچ ِ کورنو   
mârpic-e Cornu (#)

Fr.: spirale de Cornu   

A plane curve whose Cartesian coordinates are given in parametric form by the → Fresnel integrals. Cornu's spiral is an auxiliary tool for calculating the Fresnel integrals. It is particularly used for the calculation of the diffraction of light at the straight edge of a flat screen or at a straight slit. It is characterized by the fact that the angle it makes with the abscissa axis is proportional to the square of the distance along the curve from the origin of coordinates. Cornu's spiral comprises two branches, symmetrical with respect to the origin and winding asymptotically on the points (0.5,0.5) and (-0.5,-0.5) respectively. Also known as the → clothoid or Euler's spiral.

Named after the French physicist Alfred Cornu (1841-1902); → spiral.

corollary
  پسانه   
pasâné

Fr.: corollaire   

A natural outcome of a → theorem.

L.L. corollarium "a deduction, consequence," from L. corollarium, originally "money paid for a garland," hence "gift, gratuity, something extra;" from corolla "small garland," diminutive of → corona.

Pasâné, from pasân "after," from pas "after, afterward; consequently," variant pošt; Mid.Pers. pas "after; behind, before;" O.Pers. pasā "after;" Av. pasca "afterward (of time); then; behind (of space);" cf. Skt. paścā "after, later, behind;" L. post "after, afterward; behind, in the rear;" O.C.S. po "after, behind;" Lith. pas "at, by;" PIE *pos-, *posko-, + nunace suffix

corona
  تاج، هورتاج   
tâj, hurtâj (#)

Fr.: couronne   

1) The outermost atmosphere of the Sun immediately above the → chromosphere, which can be seen during a total Solar eclipse. It consists of hot (1-2 × 106 K), extremely tenuous gas (about 10-16 g cm-3) extending for millions of kilometer from the Sun's surface.
2) Meteorology: A set of one or more colored rings of small radii, concentrically surrounding the disk of the Sun, Moon, or other luminary when veiled by a thin cloud.

L. corona "crown, garland," cf. Gk. korone "anything curved, kind of crown."

Tâj "crown," loanword in Arm. tag "crown," tagavor "king," Proto-Iranian *tâgâ-, maybe from PIE base *(s)teg- "to cover" (L. toga "a garment worn by male citizens in ancient Rome;" hurtâj, from hur, → sun, + tâj.

Corona Australis
  تاج ِ هودری، ~ شمالی   
tâj-e hudari, šomâli

Fr.: Couronne australe   

The Southern Crown. A small, faint southern → constellation, also called Corona Austrini. Abbreviation: CrA, genitive: Coronae Australis.

corona; L. australis "southern."

Corona Borealis
  تاج ِ دشتری، ~ جنوبی   
tâj-e daštari, ~ jonubi

Fr.: Couronne boréale   

The Northern Crown. A small but prominent northern → constellation that lies east of → Arcturus, between → Boötes and → Hercules, and comprises a distinctive arc formed by the stars seven stars. Abbreviation: CrB; genitive: Coronae Borealis.

corona; L. borealis "northern."

coronagraph
  هورتاجنگار، تاجنگار   
hurtâjnegâr (#), tâjnegâr (#)

Fr.: coronographe   

An instrument which, when used in a telescope, produces an artificial eclipse, permitting the study of the → solar corona without a total eclipse of the Sun. It was invented in 1930 by the French astronomer Bernard Lyot (1897-1952).

From → corona + → -graph.

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