Hugoniot curve xam-e Hugoniot Fr.: courbe de Hugoniot A curve, on the pressure versus specific volume plane, representing the locus of all the possible states that can be reached by a substance immediately after the passage of a single → shock wave. For each initial condition there is a different curve. No combustion occurs in the process and, therefore, the chemical composition of the medium does not change. See also → Rayleigh line; → Crussard curve. Named after the French physicist Pierre Henri Hugoniot (1851-1887), who worked on fluid mechanics, especially flow properties before and after shock waves; → curve. |
interstellar reddening curve xam-e sorxeš-e andaraxtari Fr.: courbe de rougissement interstellaire A graph showing the relation between → interstellar absorption (in magnitudes) and wavelength. → interstellar; → reddening; → curve. |
Keplerian rotation curve xam-e carxeš-e Kepleri (#) Fr.: courbe de rotation keplérienne A → rotation curve in which the speed of the orbiting body is inversely proportional to the → square root of its distance from the mass concentrated at the center of the system. |
light curve nur-xam, xam-e nur Fr.: courbe de lumière 1) A curve showing the behavior of the light from a
→ variable star over a period of time. |
orbital phase curve xam-e fâz-e madâri Fr.: courbe de la phase orbitale The photometric variability induced by the → orbital motion in a → two-body system. |
phase curve xam-e fâz Fr.: courbe de phase 1) Astro.: A curve describing the → brightness
of a reflecting → natural satellite as a
function of its → phase angle. |
Planck curve xam-e Planck Fr.: courbe de Planck Same as → blackbody curve. |
potential energy curve xam-e kâruž-e tavand Fr.: courbe de l'energie potentielle A plot that displays the → potential energy of a moving body as a function of its position. It is explained by the → conservation of energy and the conversion of potential energy into → kinetic energy and vice versa. |
probability curve xam-e šavânâyi Fr.: courbe de probabilité A curve that describes the distribution of probability over the values of a random variable. → probability; → curve. |
radial velocity curve xam-e tondâ-ye šo'â'i Fr.: courbe de vitesse radiale A curve describing the variation of the radial velocity of a star, due to the Doppler effect, under the gravitational effect of a secondary body (companion or exoplanet). The amplitude of these variations depends upon the mass of the secondary and its distance from the star. → radial velocity; → curve. |
regression curve xam-e vâyâzeš Fr.: courbe de régression A curve representing a non-linear relationship between two or more → variables. → regression, → curve. |
response curve xam-e pâsox Fr.: courbe de réponse A curve graphically representing the magnitude of the → response of a → detector to → radiation, usually as a function of → wavelength. |
rotation curve xam-e carxeš Fr.: courbe de rotation A plot of the variation in → orbital velocity of stars and → interstellar matter with distance from the center of a → galaxy. A "flat" rotation curve indicates that the mass of the galaxy increases linearly with distance from its center. See also: farsi→ Keplerian rotation curve Rotation; → curve. |
smooth curve xam-e hamvâr Fr.: courbe lisse 1) A curve which is free from abrupt fluctuations. |
supernova light curve xam-e nur-e abarnovâ, ~ ~ abar-now-axtar Fr.: courbe de lumière de supernova The graph of luminosity as a function of time after a → supernova explosion. The → light curve goes up rapidly to a → peak luminosity, then decays away slowly over time, with different rates, depending on the → supernova type. The temporal evolution of a supernova's luminosity contains important information on the physical processes driving the explosion. The observed → bolometric light curves provide a measure of the total output of converted radiation of → Type Ia supernovae, and hence serve as a crucial link to theoretical models of the explosion and evolution. |
velocity curve xam-e tondâ Fr.: courbe de vitesse A plot of the radial velocity of an object against time, derived from the Doppler shift of spectral lines. |