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

فرهنگ ریشه شناختی اخترشناسی-اخترفیزیک

M. Heydari-Malayeri    -    Paris Observatory

   Homepage   
   


A B C D E F G H I J K L M N O P Q R S T U V W X Y Z

<< < "no abe acc act aff ama ani ant aps ast atm aut bar bic Boh bou cal car cel che cla col com com Com con con con con con con con con con con con con Cor cor cot cul de- dec dem des dif dil dir dis dom dyn Edd ele ele emi equ Eve exc exp fac fin for fre fuz gen Glo gra gra Ham hel hor hyd ign inc inf Inf int Int int ion irr jum Lag lea lig lin Lor Lyo mag mat met min Mon moo NaC neg New New non non non nul obs one opt Ori oxi par per per phl pho pla Pla pol pos pre pro pro pse qua rad rad rea rec reg rel res ret rot Ryd sci sec sec sep sim Soc son spe sta Ste Sto sub sup syn the Tho top tra Tro unc vec vio Was Wil Zhe > >>

Number of Results: 3106 Search : on
light cone
  مخروط ِ نور   
maxrut-e nur (#)

Fr.: cône de lumière   

The set of all directions in which a light signal can travel toward an event (past light cone) or from an event (future light cone).

light; → cone.

light deflection
  واچفت ِ نور   
vâcaft-e nur

Fr.: déflexion de la lumière   

The deviation of a light ray by the gravitational field of a massive body. For example, stellar light passing near the Sun will be deviated by 1''.75 at the Sun's limb.

light; → deflection.

light pollution
  آلودگی ِ نوری   
âludegi-ye nuri (#)

Fr.: pollution lumineuse   

The inappropriate or excessive use of artificial light. It brightens the sky and has a particularly damaging effect on astronomical observations. More generally, light pollution can have serious environmental consequences for humans, wildlife, and our climate. Types of light pollution include: → glare, → skyglow, → light trespass, and → light clutter.

light; → pollution.

light-second
  نور-ثانیه، ثانیه‌ی ِ نوری   
nur-sâniyé, sâniye-ye nuri

Fr.: second-lumière   

The distance travelled by light in free space in one second. It is equivalent to 2.997924580 × 108 m or 2.998 × 105 km. This unit of length is mainly used in astronomy, telecommunications, and relativistic physics. Some quantities expressed in this unit are as follows. The mean diameter of the Earth: about 0.0425 light-seconds. The average distance from the Earth to the Moon: about 1.282 light-seconds. The diameter of the Sun: about 4.643 light-seconds. The average distance from the Earth to the Sun: 499.0 light-seconds.

light; → second.

likelihood function
  کریای ِ شدواری   
karyâ-ye šodvâri

Fr.: fonction de vraisemblance   

A function that allows one to estimate unknown parameters based on known outcomes. Opposed to → probability, which allows one to predict unknown outcomes based on known parameters. More specifically, a probability refers to the occurrence of future events, while a likelihood refers to past events with known outcomes.

likelihood; → function.

limestone
  سنگ ِ آهک   
sang-e âhak (#)

Fr.: castine, calcaire    

A → sedimentary rock composed principally of calcium carbonate. Limestone is usually formed from shells of once-living organisms or other organic processes, but may also form by inorganic precipitation.

lime; → stone.

limonite
  لیمونیت   
limonit (#)

Fr.: limonite   

A widely occurring ore of yellowish-brown to black color that consists of amorphous oxides of iron.

Gk. leimon "meadow" in reference to its occurrence as "bog ore" in meadows and marshes + → -ite.

Lindblad resonance
  باز‌آوایی ِ لیندبلاد   
bâzâvâyi-ye Lindblad

Fr.: résonance de Lindblad   

A kinematic resonance hypothesized to explain the existence of galactic → spiral arms. It occurs when the frequency at which a star encounters the spiral → density wave is a multiple of its → epicyclic frequency. Orbital resonances occur at the location in the disk where Ωp = Ω ± κ/m, where Ωp is → pattern speed, κ → epicyclic frequency, and m an integer representing the number of spiral arms. The minus sign corresponds to the inner Lindblad resonance (ILR) and the plus sign to the outer Lindblad resonance (OLR). The corotation resonance corresponds to Ωp = Ω. In general, the Lindblad resonances are defined for two spiral arms (m = 2), and low order. There are other less important resonances corresponding to higher m values. These resonances tend to increase the object's orbital eccentricity and to cause its longitude of periapse to line up in phase with the perturbing force. Lindblad resonances drive spiral density waves both in galaxies (where stars are subject to forcing by the spiral arms themselves) and in Saturn's rings (where ring particles are subject to forcing by Saturn's moons).

After the originator of the model, Bertil Lindblad (1895-1965), a Swedish astronomer, who made important contributions to the study of the rotation of the Galaxy; → resonance.

line identification
  ایدانش ِ خط   
idâneš-e xatt

Fr.: identification de raies   

The process of recognizing the spectral lines in a spectrum.

line; → identification.

line of action
  خط ِ ژیرش، ~ کنش   
xatt-e žireš, ~ koneš

Fr.: ligne d'action   

Of a force, the straight line along which the force → vector is directed. The action of a force on a → rigid body does not change when its point of application is displaced along the line of action. Hence, forces applied to a rigid body can be regarded as non-localized, or sliding, vectors.

line; → action.

line of induction
  خط ِ درهازش   
xatt-e darhâzeš

Fr.: ligne d'induction   

Same as → line of force in a magnetic field.

line; → induction.

linear acceleration
  شتاب ِ خطی   
šetâb-e xatti

Fr.: accélération linéaire   

The rate of change of the → linear velocity with time. It is defined by the expression Δvt and is equal to the → first derivative of the → linear velocity.

linear; → acceleration.

linear approximation
  نزدینش ِ خطی   
nazdineš-e xatti

Fr.: approximation linéaire   

Taking the first term in the Taylor series as an approximation to a mathematical function at a given point. → first approximation.

linear; → approximation.

linear correlation
  هم‌باز‌آنش ِ خطی   
hambâzâneš-e xatti

Fr.: corrélation linéaire   

A measure of how well data points fit a straight line. When all the points fall on the line it is called a perfect correlation. When the points are scattered all over the graph there is no correlation.

linear; → correlation.

linear differential equation
  هموگش ِ دگرسانه‌ای ِ خطی   
hamugeš-e degarsâne-yi-ye xatti

Fr.: équation différentielle linéaire   

An equation in which the → dependent variable y and all its differential coefficients occur only in the first degree. A linear differential equation of → order  order n has the form:
fn(x)y(n) + fn-1(x)y(n-1) + ... + f1(x)y' + f0(x)y = Q(x),
where f0(x), f1(x), ..., fn(x) and Q(x) are each continuous functions of x defined on a common interval I and fn(x)≠ 0 in I. A linear differential equation cannot have, for example, terms such as y2 or (y')1/2. See also: → homogeneous linear differential equation; → nonhomogeneous linear differential equation.

linear; → differential; → equation.

linear equation
  هموگش ِ خطی   
hamugeš-e xatti

Fr.: équation linéaire   

An equation composed of first degree variables and representing a straight line.

linear; → equation.

linear function
  کریای ِ خطی   
karyâ-ye xatti

Fr.: fonction linéaire   

A function expressed by a → first degree equation that can be graphically represented in the → Cartesian coordinate plane by a → straight line.

linear; → function.

linear perturbation theory
  نگره‌ی ِ پرتورش ِ خطی   
negare-ye partureš-e xatti

Fr.: théorie de perturbation linéaire   

Assumption that the variations in the plasma parameters, due to the presence of waves, are small (to the first order) as compared to the undisturbed parameters. This makes it possible to linearize equations by dropping out second order (and higher) nonlinear terms.

linear; → perturbation; → theory.

linear polarization
  قطبش ِ خطی   
qotbeš-e xatti (#)

Fr.: polarisation linéaire   

Of an electromagnetic radiation, a → polarization in which the electric vibrations are confined to one plane along the direction of propagation. Also called → plane polarization. See also → circular polarization.

linear; → polarization.

linear regression
  وایازی ِ خطی   
vâyâzi-ye xatti

Fr.: regression linéaire   

In statistics, a regression method that establishes a linear relationship between two random variables.

linear; → regression.

<< < "no abe acc act aff ama ani ant aps ast atm aut bar bic Boh bou cal car cel che cla col com com Com con con con con con con con con con con con con Cor cor cot cul de- dec dem des dif dil dir dis dom dyn Edd ele ele emi equ Eve exc exp fac fin for fre fuz gen Glo gra gra Ham hel hor hyd ign inc inf Inf int Int int ion irr jum Lag lea lig lin Lor Lyo mag mat met min Mon moo NaC neg New New non non non nul obs one opt Ori oxi par per per phl pho pla Pla pol pos pre pro pro pse qua rad rad rea rec reg rel res ret rot Ryd sci sec sec sep sim Soc son spe sta Ste Sto sub sup syn the Tho top tra Tro unc vec vio Was Wil Zhe > >>