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inheritor riganbar Fr.: héritier |
inhomogeneity nâhamgeni (#) Fr.: inhomogénéité The condition or an instance of not being homogeneous. → in- "not" + → homogeneity. |
inhomogeneous nâhamgen (#) Fr.: inhomogène Lack of homogeneity; something that is not → homogeneous. → in- "not" + → homogeneous. |
initial âqâzin (#) Fr.: initial Of, pertaining to, or occurring at the beginning. Initial, from L. initialis, from initium "a beginning, an entrance," from p.p. stem of inire "to go into, begin," from → in- + ire "to go," → ion. Âqâzin "pertaing to the beginning," from âqâz "beginning," from Proto-Iranian *āgāza-, from prefix ā- + *gāz- "to take, receive," cf. Sogdian āγāz "beginning, start," pcγz "reception, taking." |
initial conditions butârhâ-ye âqâzin Fr.: conditions initiales 1) Conditions at an initial time t = t_{0} from which a physical system or
a given set of mathematical equations evolves. |
initial mass jerm-e âqâzin (#) Fr.: masse initiale The mass of a star at its arrival on the → main sequence. |
initial mass function (IMF) karyâ-ye âqâzin-e jerm Fr.: fonction initiale de masse A mathematical expression describing the relative number of stars found in different ranges of mass for a cluster of stars at the time of its formation. It is defined as φ(log M) = dN / dlog M ∝ M^{ -Γ}, where M is the mass of a star and N is the number of stars in a logarithmic mass interval. The value of the slope found by Salpeter (1955) for → low-mass and → intermediate-mass stars in the → solar neighborhood is Γ = 1.35. The IMF can be expressed also in linear mass units: χ(M) = dN / DM ∝ M^{ -α}. Note that χ(M) = (1 / M lm 10) φ(log M), and α = Γ + 1. In this formalism the Salpeter slope is α = 2.35. There is a third way for representing the IMF, in which the exponent is x = -α. The IMF is not a single power law over all masses, from → brown dwarfs to → very massive stars (Kroupa, 2002, Science 295, 82). Different slopes have been found for different mass segments, as follows: α = 1.3 for 0.08 ≤ M_{solar} < 0.5; α = 2.3 for 0.5 ≤ M_{solar} < 1; α = 2.3 for 1 ≤ M_{solar}. The IMF at low masses can be fitted by a → lognormal distribution (See Bastian et al., 2010, ARAA 48, 339 and references therein). See also → canonical IMF. |
initial phase angle zâviye-ye fâz-e âqâzin Fr.: angle de phase initial The value of the phase corresponding to the origin of time. Same as the → epoch angle. |
initial singularity takini-ye âqâzin (#) Fr.: singularité initiale An instant of infinite density, infinite pressure, and infinite temperature where the equations of general relativity break down, if the standard Big Bang theory is extrapolated all the way back to time zero. → singularity. → initial; → singularity. |
initiative bongâm Fr.: initiative 1) The first step or action of a matter; commencing move. From Fr. initiative, from L. initiatus, p.p. of initiare "to begin," from initium "a beginning," → initial. Bongâm, from bon "basis; root; foundation; bottom," → fundamental, + gâm "step, pace," → egress. |
inject daršândan Fr.: injecter 1) General: To force into a passage, cavity, or tissue. From L. injectus, p.p. of injicere "to throw in or on," from → in- "in" + -icere, combining form of jacere "to throw." Daršândan, from darešândan, from dar-, → in, + ešândan, → eject. |
injection daršâneš Fr.: injection 1) General: The act of injecting. Something that is injected. Verbal noun of → inject. |
injective daršâni Fr.: injectif Of or pertaining to a → injection. Adj. related to → injection. |
inlet šâxâbé (#) Fr.: crique, bras de mer A small arm of the sea, a lake, or a river. From → in- + let "to allow," M.E. leten, O.E. lætan; cognate with Du. laten, Ger. lassen, akin to Gk. ledein "to be weary", L. lassus "tired." Šâxâbé, literally "branch of water," from šâx, → branch, + âb "sea, river, → water" + noun suffix -é. |
inner daruni (#) Fr.: interne Situated within or farther within; interior. From O.E. inra, comparative of inne (adv.) "inside;" → in-. Daruni, adj. of darun "in, into; within" (Mid.Pers. andarôn "inside," from andar, → inter-, + rôn "side, direction;" Av. ravan- "(course of a) river"). |
inner core maqze-ye daruni Fr.: noyau interne The central part of the → Earth's core, composed of solidified → iron and → nickel, and extending from a depth of about 5100 km to the center of the Earth, at 6360 km. Its radius is about 1/3 that of the whole core and is effectively decoupled from the → mantle due to the molten nature of the surrounding → outer core. The radius of the inner core is defined by a small increase in → compressional wave velocity at a radius of about 1200 km. Its density is about 12 g/cm^{3}. The → temperature of the inner core has been estimated at 5000-7000 °C. |
inner Earth object (IEO) barâxt-e daruni-ye madâr-e zamin Fr.: objet interne à l'orbite terrestre A → near-Earth object whose → orbit lies always inside Earth's orbit. |
inner Lagrangian point noqte-ye Lagrange-e daruni (#) Fr.: point de Lagrange interne One of the five → Lagrangian points, denoted L1, which lies between the two bodies on the line passing through their center of mass. In a → close binary star system mass transfer occurs through this point. → inner; → Lagrangian points. |
inner Lindblad resonance (ILR) bâzâvâyi-ye Lindblad-e daruni Fr.: résonance de Lindblad interne A → Lindblad resonance expressed by: Ω_{p} = Ω - κ/m. → inner; → Lindblad resonance. |
inner planets sayârehâ-ye daruni (#) Fr.: planètes internes The planets Mercury, Venus, Earth and Mars collectively. T hey are also known as the terrestrial planets. |
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