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contingent âmarsân Fr.: contigent 1) Dependent for existence, occurrence, character, etc., on something not yet
certain; conditional. M.E., from M.Fr. contingent and directly from L. contingentem (nominative contingens) "happening, touching," pr.p. of contingere "to touch," → contact. Âmarsân, agent noun from *âmarsidan "to touch," related to parmâsidan "to touch, feel," → contact, Mid.Pers. marz "contact, touching," marzitan "to touch," Mod.Pers. mâlidan "to rub," Av. marəz- "to rub, wipe," marəza- "border, district," Mod.Pers. marz "border;" ultimately from Proto-Ir. *Hmars- "to touch." |
continuation peydâšt; peydâd Fr.: continuation The act or state of continuing; the state of being continued. |
continue 1) peydâštan; 2) peydâdan Fr.: continuer 1) (v.intr) To go on or keep on without interruption as in some course or action. M.E. contynuen, from O.Fr. continuer, from L. continuare "to make all one, join together, make or be continuous," from continuus "uninterrupted," from continere "to be uninterrupted," literally "to hold together," from → con- + tenere "to hold," cognate with Pers. tanidan, → tension. 1) Peydâštan,
from pey "after; pursuit; track; step," → tracking,
+ dâštan "to have, hold, maintain," → access. |
continued peydâšté Fr.: continue Continuing to happen or exist for a long time. Occurring many times. Past participle of → continue. |
continued fraction barxe-ye peydâšté Fr.: fraction continue In mathematics, a fraction whose numerator is an integer and whose denominator is an integer plus a fraction whose numerator is an integer and whose denominator is an integer plus a fraction and so on. |
continuous peyvasté (#) Fr.: continu 1) General: Uninterrupted in extent, sequence, or time. From L. continuus "uninterrupted," from contin(ere) "to hold together, retain," → continue, + -uus verbal adj. suffix. Peyvasté "continous," peyvastan "to connect, join," Mid.Pers. paywastan, from *pati-basta-, from suffix pati- (Mid.Pers. pât-,from O.Pers. paity "agaist, back, opposite to, toward, face to face, in front of," Av. paiti, akin to Skt. práti "toward, against, again, back, in return, opposite," Pali pati-, Gk. proti, pros "face to face with, toward, in addition to, near;" PIE *proti) + basta- "tied, shut" (Av./O.Pers. band- "to bind, fetter," banda- "band, tie," Skt. bandh- "to bind, tie, fasten," PIE *bhendh- "to bind," cf. Ger. binden, E. bind), cf. Skt. prati-bandh- "to tie." |
continuous data dâdehâ-ye peyvasté Fr.: données continues Data that can take any value along a continuum (e.g. air temperature between two upper and lower boundaries) as opposed to → discrete data, which can only take integer values. → continuous; → data. |
continuous function karyâ-ye peyvasté Fr.: fonction continue The function y = f(x) is called continuous at the point x = x_{0} if it is defined in some neighborhood of the point x_{0} and if lim Δy = 0 when Δx → 0. → continuous; → function. |
continuous spectrum binâb-e peyvasté Fr.: spectre continu An electromagnetic spectrum in which emitted or absorbed radiation is present continuously over all wavelengths in a given range. → continuous; → spectrum. Binâb, → spectrum; peyvasté→ continuous. |
continuous variable vartande-ye peyvasté Fr.: variable continu A variable which has changes continuously, in contrast to → discrete variables. → continuous; → variable. |
continuous-time quantum walk puyeš-e kuântomi bâ zamân-e peyvasté Fr.: marche quantique à temps continu A → quantum walk taking place entirely in the position space. Continuous-time quantum walk was introduced by E. Farhi & S. Gutmann (1998, Phys. Rev. A 58, 915). → continuous; → time; → quantum; → walk. |
continuum peyvastâr (#) Fr.: continuum A continuous extent or succession, which has no discrete parts, as the continuum of real numbers as opposed to the sequence of discrete integers. → continuum emission. From L. neut. of continuus, → continuous Peyvastâr, from peyvast past tense stem of peyvastan "to connect, join," Mid.Pers. paywastan, from *pati-basta-, from suffix pati- (Mid.Pers. pât-, from O.Pers. paity "agaist, back, opposite to, toward, face to face, in front of," Av. paiti, akin to Skt. práti "toward, against, again, back, in return, opposite," Pali pati-, Gk. proti, pros "face to face with, toward, in addition to, near;" PIE *proti) + basta- "tied, shut" (Av./O.Pers. band- "to bind, fetter," banda- "band, tie," Skt. bandh- "to bind, tie, fasten," PIE *bhendh- "to bind," cf. Ger. binden, E. bind), cf. Skt. prati-bandh- "to tie." + -âr suffix forming verbal noun. |
continuum emission gosil-e peyvastâr Fr.: émission continuum A continuous radiation produced by three processes: radiative recombination due to transition between electron free-free states, two-photon decays of metastable levels, and thermal bremsstrahlung. → continuum; → emission. |
continuum-driven wind bâd-e peyvastârzâd Fr.: vent induit par continuum The transfer of photon momentum to free electrons. The acceleration by → continuum emission can be given by: a_{c} = (σ/m)(L_{*}/4πR^{2}c), where σ is the → Thomson scattering → cross section, m is the mass per free electron, L_{*} is → stellar luminosity, R_{*} is radius, and c the → speed of light. The ratio of a_{c} to the → surface gravity is ≅ 2 × 10^{-5}L_{*}/M_{*}, with M_{*} and L_{*} in solar units. The atmosphere is is stable if a_{c} very smaller than g_{grav}. If L_{*} is above the → Eddington limit, the radiation pressure in the continuum leads to very heavy → mass loss and thus to expanding envelopes (K.S. de Boer & W. Seggewiss, 2008, Stars and Stellar Evolution, EDP Sciences). |
convective overshooting farâzad-e hambazi Fr.: dépassement convectif In a → massive star, penetration of the upper layers of the → convective core into the → radiative zone due to → turbulence effects. The enlargement of the convective core results in more luminous stars in theoretical models. → convective; → overshooting. |
core overshooting farâzad-e maqzé Fr.: dépassement du cœur → core; → overshooting. |
corotating interaction region (CIR) nâhiye-ye andaržireš-e hamcarxandé Fr.: région d'interaction en corotation A spiral-shaped density enhancement formed around a star when fast stellar winds collide with slower material. This large-scale wind structure can extend from the stellar surface to possibly several tens of stellar radii. The CIRs can be produced by intensity irregularities at the stellar surface, such as dark and bright spots, magnetic loops and fields, or non-radial pulsations. The surface intensity variations alter the radiative wind acceleration locally, which creates streams of faster and slower wind material. CIRs are responsible for the → discrete absorption components seen in some ultraviolet → resonance lines of → hot stars (S. R. Cranmer & S. P. Owocki, 1996, ApJ 462, 469). → corotate; → interaction; → region. |
correcting plate tiqe-ye aršâyandé, ~ aršâgar Fr.: lame correctrice A large glass plate placed at the entrance of a Schmidt telescope to correct for spherical aberration over the large field of view. |
Cretaceous-Paleogene extinction event ruydâd-e xâmuši-ye Gacâsâ-Pârinzâd Fr.: extinction Crétacé-Tertiaire The → mass extinction event that destroyed the dinosaurs and a majority of other species on Earth approximately 65 million years ago. This event is believed to have been the impact of a 10 km-size → asteroid or → comet nucleus and its aftereffects, including a severe → impact winter. The collision would have released the energy equivalent to 100 million megatonnes (teratonnes) of → TNT, i.e. more than 10^{9} times the energy of the atomic bomb dropped on Hiroshima on August 6, 1945. Same as the → Cretaceous-Tertiary event. → Cretaceous; → Paleogene; → extinction; → event. |
curve fitting saz-e xam, sazkard-e ~ Fr.: ajustement de courbe Construction of mathematical functions whose graphs are curves that "best" approximate a given collection of data points. |
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