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Planck's radiation law
qânun-e tâbeš-e Planck
Fr.: loi du rayonnement de Planck
An equation that expresses the energy radiated per unit area per unit time per unit wavelength range by a blackbody as a function of temperature. It is expressed by → Planck's blackbody formula.
1) hâmon (#); 2) taxt (#)
1) (n.) a flat or level surface.
1) From L. plantum "flat surface," noun use of adj. planus "flat,
1) Hâmon, variant of hâmun "plain, level ground;" Mid.Pers. hâmôn
"level, flat;" Proto-Iranian *hāma-van-,
*hāma- "same, equally, even; together, with" (Mod.Pers./Mid.Pers.
ham-; cf. Skt. sam-; also O.Pers./Av. hama-
"one and the same;" Skt. sama-; Gk. homos-;
originally identical with PIE numeral *sam-
"one," from *som-. The Av. ham- appears in various forms:
han- (before gutturals, palatals, dentals) and also hem-,
hen-) + *-van- suffix.
šekl-e hâmon, ~ taxt
Fr.: figure plane
A two-dimensional geometric figure. The points of the figure lie entirely in a plane.
âyene-ye taxt (#)
Fr.: miroir plan
A mirror whose reflective surface is neither concave nor convex.
plane of polarization
Fr.: plan de polarisation
In a → linearly polarized light, a plane perpendicular to the → plane of vibration and containing the direction of propagation of light. It is also the plane containing the direction of propagation and the magnetic vector (H) of the electromagnetic light wave.
plane of rotation
Fr.: plan de rotation
plane of the sky
Fr.: plan du ciel
An imaginary plane that is perpendicular to the → line of sight.
plane of vibration
Fr.: plan de vibration
In a → linearly polarized light, a plane perpendicular to the → plane of polarization and containing the direction of propagation of light. It is also the plane containing the direction of propagation and the electric vector (E) of the electromagnetic light wave.
Fr.: polarisation plane
Same as → linear polarization.
plane polarized light
nur-e qotbide-ye hâmoni
Fr.: lumière polarisée plane
mowj-e taxt (#)
Fr.: onde plane
A wave whose wavefronts of constant phase are infinite parallel planes normal to the direction of propagation.
havâsepehr-e parâsu-taxthâ, javv-e ~
Fr.: atmosphère plan-parallèle
An approximation used in many stellar atmosphere models that depict the atmosphere as being only one-dimensional and bounded at the top and bottom by horizontal plane surfaces normal to the direction of gravity.
Fr.: lame plan-parallèle
A piece of glass with plane parallel surfaces used to admit light into an optical system and to exclude dirt and moisture.
1) A celestial body that: (a) is in orbit around the Sun, (b) has
sufficient mass for its self-gravity to overcome rigid body forces so
that it assumes a hydrostatic equilibrium (nearly round) shape, and
(c) has cleared the neighborhood around its orbit.
→ dwarf planet.
From O.E., from O.Fr. planete (Fr. planète), from L.L. planeta (plural form planetae), from Gk. planetes (single form) "wandering," from (asteres) planetai "wandering (stars)," from planasthai "to wander," of unknown origin.
Sayyâré, from Ar. saiyârat "walker, traveller."
Fr.: Planète Neuf
A hypothetical large planet in the far outer → solar system the gravitational effects of which would explain the unexpected orbital configuration of a group of → trans-Neptunian objects (TNOs). Trujillo & Sheppard (2014) noticed a clustering of the → argument of perihelion of bodies lying beyond ~150 → astronomical unit (AU), and attributed this to a hypothetical super-Earth body lying at several hundred AUs. Batygin & Brown (2016) showed numerically and analytically how the apsidal and nodal clustering of the distant TNOs arises as a result of resonant and secular dynamical effects from a distant perturber. They identified a range of semimajor axes (400-1500 AU) and eccentricities (0.5-0.8) for which a distant planet can explain the → orbital elements of the distant TNOs. The predicted planet would have a mass of 10 Earths (approximately 5,000 times the mass of → Pluto), a diameter of four times Earth and a highly elliptical orbit with an → orbital period of approximately 15,000 years.
1) âsmânnemâ; 2) âsmânxâné (#)
1) A device that produces a representation of the heavens by the use of a number of
From → planet + -arium "a place for."
&ACIRC;smânnemâ, literally "sky displayer," from
âsmân "sky" (Mid.Pers. âsmân "sky, heaven;"
"heaven;" Av. asman- "stone, sling-stone; heaven;" cf. Skt. áśman-
"stone, rock, thunderbolt;" Gk. akmon "heaven, meteor, anvil;" Akmon
was the father of Ouranos (Uranus), god of sky; Lith. akmuo "stone;" Rus. kamen;
PIE base *akmon- "stone, sky."
The link between the "stone" and "sky" concepts indicates that the sky had once been conceived
as a stone vault by prehistoric Indo-Europeans) +
nemâ "displayer," from
nemudan "to show" (Mid.Pers. nimūdan, nimây-
"to show," from O.Pers./Av. ni- "down; into"
(Skt. ni "down," nitaram "downward," Gk. neiothen "from below,"
cf. E. nether, O.E. niþera, neoþera "down, downward, below, beneath," from
Du. neder, Ger. nieder; PIE *ni- "down, below") + māy-
"to measure;" cf. Skt. mati "measures," matra- "measure;"
Gk. metron "measure;" L. metrum;
PIE base *me- "to measure").
Of, pertaining to, or resembling a planet or planets.
Fr.: aberration planétaire
The difference between the true position of a planet and its apparent position, due to the time required for light to travel the distance from the planet to Earth. Correction for planetary aberration is necessary in determining orbits.
Fr.: nébuleuse planétaire
A hot envelope of gas ejected from a central evolved star before becoming a → white dwarf. At the end of the → asymptotic giant phase the pulsating → red giant star is surrounded by an extended shell formed by the material ejected from it. As the evolved star contracts, its → effective temperature rises considerably. When it reaches about 30,000 K, the radiated photons become energetic enough to ionize the atoms in the nebula. The nebula becomes then visible in the optical. It shines essentially in a few → emission lines, produced by cascades during recombination or by collisional excitation with electrons. The central stars of planetary nebulae, → CSPNe, are typically 0.6 to 0.8 solar masses. They have → main sequence masses in the range 1 to 8 solar masses, with an average mass of 2.2 solar masses for a standard → initial mass function. Thus a total of about 1.6 solar masses is in average lost during the → AGB and planetary nebula phases. The life-time of planetary nebulae is relatively short. A typical planetary nebula lasts only a few 10,000 years.
→ planetary; → nebula. The name comes from the fact that these objects appear as planetary disks in a low-resolution telescope. The first planetary nebula, designated NGC 7009 or the → Saturn Nebula, was discovered in 1782 by the German-born English astronomer William Herschel (1738-1822), who described it as "planetary nebula."