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Number of Results: 471 Search : ity

isoplanicity 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 → → |

Jeans instability nâpâydâri-ye Jeans Fr.: instabilité de Jeans An instability that occurs in a → → |

Kelvin-Helmholtz instability nâpâydâri-ye Kelvin-Helmholtz (#) Fr.: instabilité de Kelvin-Helmholtz An → |

Keplerian angular velocity 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:
Ω |

Keplerian orbital velocity tondâ-ye madâr-e Kepleri Fr.: vitesse d'orbite képlérienne The velocity of an object orbiting another object according to
→ |

kinematic viscosity vošksâni-ye jonbešik Fr.: viscosité cinématique The ratio of the → |

kinetic helicity 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
→ .
In the absence of magnetic field, this quantity is conserved by the
→ u)Euler equation. See also
→ magnetic helicity. |

Kramers' opacity law qânun-e kederi-ye Kramers (#) Fr.: loi de l'opacité de Kramers Same as → Named after Henrik Kramers (1894-1952); → |

Lagrangian density cagâli-ye Lagranži Fr.: densité lagrangienne A quantity, denoted Lagrangian formalism, and defined as the
→ Lagrangian per unit volume.
It is related to the Lagrangian L by: L = ∫∫∫L d_{d}^{3}V. Lagrangian density is often called Lagrangian when there is no ambiguity. → |

law of identity qânun-e idâni Fr.: principe d'identité Same as → |

line intensity 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 profile variability (LPV) vartandegi-ye farâpâl-e xatt Fr.: variabilité du profil de raie The change in the shape of a → → |

linear instability nâpâydâri-ye xatti (#) Fr.: instabilité linéaire An instability that can be described (to first-order accuracy) by linear (or tangent linear) equations. → |

linear velocity 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 → ω ×.r |

linearity xattigi Fr.: linéarité The property, condition, or state of being linear. |

low-metallicity environment pargir-e kamfelez Fr.: environnement faible en métaux A medium in which chemical elements have abundances smaller than the solar values. → |

luminosity tâbandegi (#) Fr.: luminosité The → Verbal noun of → |

luminosity class rade-ye tâbandegi (#) Fr.: classe de luminosité A classification of stellar spectra according to luminosity for a
given → → |

luminosity distance apast-e tâbandegi Fr.: distance de luminosité 1) Distance derived by comparison of → 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 (D_{A})
by:
D_{L} = (1 + z)^{2}.D_{A}.→ |

luminosity function karyâ-ye tâbandegi Fr.: fonction de luminosité Number → → |

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