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speech 1) soxan (#); 2) soxanrâni (#) Fr.: 1) parole; 2) discours, allocution 1) The faculty or power of speaking; oral communication; ability to
express one's thoughts and emotions by speech sounds and gesture (Dictionary.com). M.E. speche; O.E. spæc; cf. Dan. sprog, O.S. spraca, O.Fris. spreke, Du. spraak, O.H.G. sprahha, Ger. Sprache "speech." Soxan "speech, utterance, word;" Mid.Pers. saxwan "word, speech;" O.Pers. θa^{n}h- "to declare, say," aθaham "I said;" Av. səngh- "to declare," sənghāmi "I say;" cf. Skt. śams- "to praise, declare;" L. censere "to estimate, think; decide." |
speed tondi (#) Fr.: vitesse The ratio of the distance covered to the time taken by a moving body. Speed in a specified direction is → velocity. M.E. spede "good luck, prosperity, rapidity;" O.E. sped "success, prosperity, advancement;" cf. O.S. spod "success," Du. spoed "haste, speed," O.H.G. spuot "success," O.H.G. spuoten "to haste;" from PIE base *spe- "to thrive, prosper" (cf. Skt. sphā- "to increase, become fat;" L. sperare "to hope;" O.C.S. spechu "endeavor;" Lith. speju "to have leisure"). Tondi "speed," from tond "swift, rapid, brisk; fierce, severe" (Mid.Pers. tund "sharp, violent;" Sogdian tund "violent;" cf. Skt. tod- "to thrust, give a push," tudáti "he thrusts;" L. tundere "to thrust, to hit" (Fr. percer, E. pierce, ultimately from L. pertusus, from p.p. of pertundere "to thrust or bore through;" PIE base *(s)teud- "to thrust, to beat") + noun suffix -i. |
speed of light tondi-ye nur Fr.: vitesse de la lumière Same as → velocity of light. |
spend ziyâmidan Fr.: dépenser 1) To pay out, disburse, or expend; dispose of (money, wealth, resources, etc.). M.E. spenden, from O.En. -spendan (in forspendan "use up"), from M.L. spendere, from expendere "to pay out, weigh out money," from → ex- "out" + pendere "to pay, weigh." Ziyâmidan, from Sogd. zyâm "to consume, spend," ultimately from Proto-Ir. *uz-iam-, from *uz- "out, away," → ex-, + *iam- "to hold, take; stretch, reach out;" cf. Av. yam- "to hold, keep," (+ *apa-) "to take away;" Skt. yam- "to hold, restrain." |
sphere koré (#), sepehr (#) Fr.: sphère A solid geometric figure generated by the revolution of a semicircle about its diameter; equation: x^{2} + y^{2} + z^{2} = r^{2}. M.E. spere, from O.Fr. espere, from L. sphæra "globe, ball, celestial sphere," from Gk. sphaira "globe, ball," of unknown origin. Koré, loan from Ar. kurat. |
sphere of influence sepehr-e hanâyeš Fr.: sphère d'influence The region of space around one of the bodies in a system of two celestial bodies where a third body of much smaller mass is influenced by the gravitational field of that body. The sphere of influence of a planet with respect to the Sun has a radius given by: R = R_{P}(M_{P}/M_{S})^{2/3}, where R_{P} is the radius of the planet's orbit around the Sun, M_{P} is the mass of the planet, and M_{S} is the solar mass. The sphere of influence of the Earth has a radius of about 927,000 km or slightly under 150 Earth radii. Beyond this limit, a space probe will come under the influence of the Sun. |
spheres of Eudoxus sepehrhâ-ye Eudoxus Fr.: sphères d'Eudoxe A series of spheres with varying radii centred on the Earth, each rotating uniformly about an axis fixed with respect to the surface of the next larger sphere, all comprising a model in Greek astronomy to describe the motions of the heavenly bodies. The spheres turned with different speeds about axes with different orientations. The fixed stars revolved around the Earth by the motion of the most distant sphere to which the stars were thought to be attached. Each of the five planets' (Mercury, Venus, Mars, Jupiter, and Saturn) motion could be described using four spheres. The Sun and the Moon required three spheres each to explain their motions. Therefore, a total of 27 spheres described the behavior of the heavenly bodies in terms of circular motion. Eudoxus was the first person to devise a model that could explain the → retrograde motion of the planets in the sky along a looped curve known as the → hippopede. → sphere; Eudoxus (Ευδοξοσ) of Cnidus (c 408 BC - c 355 BC), Greek astronomer and mathematician. |
spherical kore-yi Fr.: sphérique Having the form of a sphere; of or pertaining to a sphere or spheres. |
spherical aberration birâheš-e koreyi Fr.: aberration sphérique, ~ de sphéricité An aberration of a spherical lens or mirror in which light rays converge not to a single point but to a series of points with different distances from the lens or mirror. Spherical aberration is corrected by using parabolic reflecting and refracting surface → spherical; → aberration. |
spherical angle zâviye-ye koreyi Fr.: angle sphérique An angle formed on the surface of a sphere by the intersection of two great circles of the sphere. |
spherical astrolabe ostorlâb-e sepehri, ~ kore-yi Fr.: astrolabe sphérique A type of → astrolabe in which the observer's horizon is drawn on the surface of a globe, mounted with a freely rotating spherical lattice work or 'spider' representing the celestial sphere. The earliest description of the spherical astrolabe dates back to the Iranian astronomer Nayrizi (865-922). |
spherical astronomy axtaršenâsi-ye kore-yi Fr.: astronomie sphérique The branch of astronomy that is concerned with determining the apparent positions and motions of celestial bodies on the celestial sphere. Same as → positional astronomy. |
spherical coordinates hamârâhâ-ye kore-yi Fr.: coordonnées sphériques A coordinate system using an origin (O) and three perpendicular axes (Ox, Oy, Oz), in which the position of a point (P) is given by three numbers (r, θ, φ). The coordinate r is the distance from the origin, θ the angle between the z-axis and the r direction, and φ the angle between the projection of r on the xy-plane and the Ox-axis. The coordinate φ is also called the → azimuthal angle. → spherical; → coordinate. |
spherical excess fozuni-ye sepehri, ~ kore-yi Fr.: excès sphérique The difference between the sum of the three angles of a → spherical triangle and 180° (π radians). |
spherical geometry hendese-ye kore-yi Fr.: géométrie sphérique The branch of geometry that deals with figures on the surface of a sphere (such as the spherical triangle and spherical polygon). It is an example of a non-Euclidean geometry. |
spherical harmonic hamâhang-e kore-yi Fr.: fonction harmonique sphérique A solution of some mathematical equations when → spherical polar coordinates are used in investigating physical problems in three dimensions. For example, solutions of → Laplace's equation treated in spherical polar coordinates. Spherical harmonics are ubiquitous in atomic and molecular physics and appear in quantum mechanics as → eigenfunctions of → orbital angular momentum. They are also important in the representation of the gravitational and magnetic fields of planetary bodies, the characterization of the → cosmic microwave background anisotropy, the description of electrical potentials due to charge distributions, and in certain types of fluid motion. The term spherical harmonics was first used by William Thomson (Lord Kelvin) and Peter Guthrie Tait in their 1867 Treatise on Natural Philosophy; → spherical; → harmonic. |
spherical latitude varunâ-ye kore-yi, ~ sepehri Fr.: latitude sphérique The angle between the → normal to a spherical reference surface and the → equatorial plane. |
spherical polar coordinate hamârâhâ-ye kore-yi-ye qotbi Fr.: coordonnées sphériques polaires Same as → spherical coordinates. → spherical; → polar; → coordinate |
spherical symmetry hamâmuni-ye kore-yi Fr.: symétrie sphérique A configuration in which the constituting parts are arranged concentrically around the center of a sphere. |
spherical triangle sebar-e kore-yi Fr.: triangle sphérique A triangle drawn on the → surface of a → sphere. A spherical triangle, like a plane triangle, may be right, obtuse, acute, equilateral, isosceles, or scalene. The sum of the angles of a spherical triangle is greater than 180° (π) and less than 540° (3π). See also → spherical excess. |
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