Fr.: terme d'advection
The first term on the right side in the → induction equation.
An agent or factor that determines the nature of something or that fixes or
conditions an outcome.
From → determine + -ant suffix forming noun.
The act of deciding definitely and firmly; the result of such an act of decision.
Verbal noun of → determine.
1) General: To settle or decide by choice of alternatives or possibilities.
Âtarmidan, from âtarm + verb forming suffix -idan; âtarm from intensive prefix â- + tarm "limit, boundary," → term.
1) Decided; settled; resolved.
p.p. of → determine.
The belief that every event is necessitated by antecedent events and conditions together with the laws of nature. → deterministic physics.
Âtarmbâvari, from âtarm, → determine, + bâvari, noun of bâvar "beleif;" Mid.Pers. wâbar "beleif;" Proto-Iranian *uar- "to choose; to convince; to believe;" cf. Av. var- "to choose; to convince" varəna-, varana- "conviction, faith;" O.Pers. v(a)r- "to choose; to convince;" Skt. vr- "to choose," vara- "choosing."
Of, pertaining to, or dealing with → determinism.
From determinist + → -ic.
Fr.: physique déterministe
The classical representation of the laws of nature according to which a particular future state (B) will arise from a particular past one (A). In contrast to → quantum physics which deals with the probability for the transition from A to B.
Deterministic, adj. of determinism; → physics.
Fr.: théorie déterministe
A theory in which specification of the initial value of all relevant variables of the system is sufficient to calculate the past values and to predict the future values of such variables for any arbitrary time. Moreover, it is possible, for any arbitrary time, to assign a value to all the variables characterizing the system. In quantum mechanics, the time evolution of the → wave function, governed by the → Schrodinger equation, is deterministic. Quantum mechanics, however, is a non deterministic theory because of the probabilistic nature of the predictions for the values of the → observables of a quantum system.
e-term of aberration
birâheš-e tarm-e e
Fr.: aberration elliptique
The same as → elliptic aberration.
Philosophy: The doctrine that there are events which do not correspond with
determinism and therefore are uncaused in some sense.
Nâtarmbâvari, nâtarmvari, from nâ- negation prefix + (â)tarmbâvari, (â)tarmvari, → determinism.
myiâni (#), andarmiyâni (#), miyânji (#)
1) (Adj.) Being or acting at the middle place or stage, or between extremes.
Intermediate, from M.L. intermediatus "lying between," from L. intermedius "that which is between," from → inter- "between" + medius "located in the middle;" PIE root *medhyo- "middle;" cf. Pers. miyân, as below; Av. maidiia-, Skt. mádhya-; Gk. medos, messos "middle;"
Miyâni, adj. of miyân "within, between, center," from
Mid.Pers. mayân "middle; among, between," Av. maidiia- "middle, the middle,"
maiδiiāna- "middle, center;" cf. Skt. mádhya-
"middle, located in the middle;" G.H.G. mitti "located in the middle."
Fr.: boson intermédiaire
A hypothetical → elementary particle that mediates the → weak interaction, carrying its effect from one particle to another as the photon does for electromagnetic interactions. First introduced in 1961 by Sheldon Glashow.
Fr.: fréquence intermédiare
forusorx-e miyâni (#)
Fr.: infrarouge moyen
intermediate-mass black hole (IMBH)
siyah câl-e miyân jerm
Fr.: trou noir de masse intermédiaire
A → black hole with a mass in the range 102-104 solar masses. IMBHs may form as the result of multiple → mergers of smaller objects in the centers of dense stellar clusters in the present universe, assuming → mass loss from → stellar winds is not significant. They may also arise from the evolution of → very massive stars early in the history of the Universe, forming black hole "seeds" in the centers of massive halos (the precursors of the galaxies we see today) early in the history of the Universe, to redshifts z > 10. Currently the best observational evidence for IMBHs comes from models of ultraluminous X-ray sources (See, e.g., J. M. Centrella et al. 2010, astro-ph/1010.5260).
Fr.: protoétoile de masse intermédiare
A protostar that evolves into an → intermediate-mass star.
Fr.: étoile de masse intermédiare
A star whose mass lies in the range about 2 to 8 → solar masses approximately.
A property of a turbulent dynamical system which is characterized by chaotic, irregular behavior occurring between quiet (or less irregular) periods. In other words, a → turbulent flow having a large → Reynolds number undergoes a phenomenon in which its turbulent activity at a fixed location stops from time to time and starts again. In fact → turbulence never completely disappears, but it can become extremely weak interrupted irregularly by bursts of strong turbulence (see also → developed turbulence). For intermittent flows → probability density functions are not → Gaussian. Turbulent intermittency plays a fundamental role in fields ranging from combustion physics, chemical engineering, meteorology, to astrophysical systems, more specifically the → interstellar medium.
From L. intermittent, pr.p. of intermittere "to leave a space between, drop (for a while), leave off," from → inter- + mittere "to send, let go."
Raftomând, literally "to go and to stop," from raft past stem of raftan "to go, walk, proceed" (present stem row-); Mid.Pers. raftan, raw-, Proto-Iranian *rab/f- "to go; to attack") + -o- euphonic infix + mând past stem of mândan "to remain, stay, relinquish, leave" (Mid.Pers. mândan "to remain, stay," mân "house, home;" O.Pers. mān- "to remain, dwell;" Av. man- "to remain, dwell; to wait;" cf. Gk. menein "to remain;" L. manere "to stay, remain, abide," mansio "a staying, a remaining, night quarters, station" (Fr. maison, ménage; E. manor, mansion, permanent; PIE *men- "to remain, wait for").
Alternately ceasing and beginning again; adj. of → intermittency.
Adjective of → intermittency.