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: 471 Search : ity
isoplanicity
  ایزوبیراهیگی   
izobirâhigi

Fr.: isoplanicité   

The condition in which the wavefronts arriving from different parts of a region of sky undergo almost identical phase perturbations. See also → isoplanatic patch.

isoplanatic; → patch.

Jeans instability
  ناپایداری ِ جینز   
nâpâydâri-ye Jeans

Fr.: instabilité de Jeans   

An instability that occurs in a → self-gravitating  → interstellar cloud which is in → hydrostatic equilibrium. Density fluctuations caused by a perturbation may condense the material leading to the domination of gravitational force and the cloud collapse. The advent of instability involves a threshold called the → Jeans length or the → Jeans mass.

Jeans; → instability.

Kelvin-Helmholtz instability
  ناپایداری ِ کلوین-هلمهولتس   
nâpâydâri-ye Kelvin-Helmholtz (#)

Fr.: instabilité de Kelvin-Helmholtz   

An → instability raised when there is sufficient velocity difference across the interface between two uniformly moving → incompressible fluid layers, or when velocity → shear is present within a continuous fluid.

Kelvin-Helmholtz contraction; → instability.

Keplerian angular velocity
  تندای ِ زاویه‌ای ِ کپلری   
tondâ-ye zâviye-yi-ye Kepleri

Fr.: vitesse angulaire keplérienne   

The angular velocity of a point in a circular orbit around a central mass. It is given by: ΩK = (GM/r3)1/2, where G is the → gravitational constant, M is the mass of the gravitating object, and r is the radius of the orbit of the point around the object.

Keplerian; → angular; → velocity.

Keplerian orbital velocity
  تندای ِ مدار ِ کپلری   
tondâ-ye madâr-e Kepleri

Fr.: vitesse d'orbite képlérienne   

The velocity of an object orbiting another object according to → Kepler's laws.

Keplerian; → orbital; → velocity.

kinematic viscosity
  وشکسانی ِ جنبشیک   
vošksâni-ye jonbešik

Fr.: viscosité cinématique   

The ratio of the → dynamic viscosity (η) to the density (ρ) of a fluid: ν = η/ρ. The unit of kinematic viscosity in the → SI system is m2s-1. In the → cgs system, cm2s-1, equal to 10-4 m2s-1, is called the → stokes (st).

kinematic; → viscosity.

kinetic helicity
  پیچاری ِ جنبشی   
picari-ye jonbeši

Fr.: hélicité cinétique   

In fluid mechanics, a quantity that describes helical flow. It is defined by the integrated scalar product of the velocity field and the → vorticity: KK = ∫ dVu . ( x u). In the absence of magnetic field, this quantity is conserved by the → Euler equation. See also → magnetic helicity.

kinetic; → helicity.

Kramers' opacity law
  قانون ِ کدری ِ کرامرز   
qânun-e kederi-ye Kramers (#)

Fr.: loi de l'opacité de Kramers   

Same as → Kramers' law.

Named after Henrik Kramers (1894-1952); → law.

Lagrangian density
  چگالی ِ لاگرانژی   
cagâli-ye Lagranži

Fr.: densité lagrangienne   

A quantity, denoted Ld, describing a continuous system in the → Lagrangian formalism, and defined as the → Lagrangian per unit volume. It is related to the Lagrangian L by:
L = ∫∫∫Ld d3V.
Lagrangian density is often called Lagrangian when there is no ambiguity.

Lagrangian; → density.

law of identity
  قانون ِ ایدانی   
qânun-e idâni

Fr.: principe d'identité   

Same as → principle of identity.

law; → identity.

line intensity
  درتنویی ِ خط   
dartanuyi-ye xatt

Fr.: intensité de raie   

A measure of the total effect of an absorption or emission line. The line intensity is equal to the integration of the absorption coefficient over the entire shape of the absorption line.

line; → intensity.

line profile variability (LPV)
  ورتندگی ِ فراپال ِ خط   
vartandegi-ye farâpâl-e xatt

Fr.: variabilité du profil de raie   

The change in the shape of a → spectral line over time. For instance, in → Wolf-Rayet stars the line profile varying on time-scales of minutes to hours is attributed to → microturbulence.

line; → profile; → variability.

linear instability
  ناپایداری ِ خطی   
nâpâydâri-ye xatti (#)

Fr.: instabilité linéaire   

An instability that can be described (to first-order accuracy) by linear (or tangent linear) equations.

linear; → instability.

linear velocity
  تندای ِ خطی   
tondâ-ye xatti

Fr.: vitesse linéaire   

The rate of change of the position of an object that is traveling along a straight path. In other words, the velocity of an object when its moving direction is not changing. For a given → angular velocity (ω), the linear velocity v of the particle is directly proportional to the distance of the particle from the center of the circular path: v = ω ×r.

linear; → velocity.

linearity
  خطیگی   
xattigi

Fr.: linéarité   

The property, condition, or state of being linear.
Math.: A relationship between two variables so that when plotted on a graph they yield a straight line.

linear; → -ity.

low-metallicity environment
  پرگیر ِ کم‌فلز   
pargir-e kamfelez

Fr.: environnement faible en métaux   

A medium in which chemical elements have abundances smaller than the solar values.

low; → metallicity; → environment.

luminosity
  تابندگی   
tâbandegi (#)

Fr.: luminosité   

The → total → brightness of a star or other astronomical object. It is expressed in watts and represents the total amount of → energy that the object radiates each → second over all wavelength regions of the → electromagnetic spectrum. Because this quantity is independent of distance, it is an → intrinsic brightness.
See also:
absolute luminosity, → anomalous luminosity effect, → bolometric luminosity, → color-luminosity diagram, → Eddington luminosity, → H II region luminosity, → intrinsic luminosity, → luminosity class, → luminosity distance, → luminosity function, → luminosity problem, → luminosity-size relation, → mass-luminosity ratio, → mass-luminosity relation, → peak luminosity, → period-luminosity relation, → solar luminosity, → stellar luminosity, → wind luminosity.

Verbal noun of → luminous.

luminosity class
  رده‌ی ِ تابندگی   
rade-ye tâbandegi (#)

Fr.: classe de luminosité   

A classification of stellar spectra according to luminosity for a given → spectral type. The luminosity class is an indication of a star's → surface gravity. It is shown by a Roman numeral as follows: I (→ supergiants), II (bright → giants), III (normal giants), IV (→ subgiants), and V (→ dwarf stars, or → main-sequence stars). Luminosity classes VI (→ subdwarfs) and VII (→ white dwarfs) are rarely used. Subclasses a, b, and c are especially used for supergiants, while the most luminous → hypergiants are assigned luminosity class Ia-0.

luminosity; → class.

luminosity distance
  اپست ِ تابندگی   
apast-e tâbandegi

Fr.: distance de luminosité   

1) Distance derived by comparison of → observed and → intrinsic luminosities. If an object has a known luminosity L, and the observed flux is S, the luminosity distance is defined by DL = (L/4πS)1/2.

2) In cosmology, the → expansion of the Universe results in a diminution of the photon flux and the above equation fails. The reason is that for a homogeneous and isotropic Universe (→ Robertson-Walker metric), the luminosity decreases by a factor (1 + z)4. Therefore, the luminosity distance is related to the → angular diameter distance (DA) by: DL = (1 + z)2.DA.

luminosity; → distance.

luminosity function
  کریا‌ی ِ تابندگی   
karyâ-ye tâbandegi

Fr.: fonction de luminosité   

Number → distribution of → stars or galaxies (→ galaxy) with respect to their → absolute magnitudes. The luminosity function shows the → number of stars of a given intrinsic luminosity (or the number of galaxies per integrated magnitude band) in a given → volume of space.

luminosity; → function.


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