Past participle of → resolve.
Fr.: raie résolue
A → spectral line that is not contaminated by other nearby lines.
Fr.: pouvoir de résolution, pouvoir séparateur
A measure of an optical system's ability to produce an image which separates two points or parallel lines on the object.
Fr.: solution saturée
A solution which can exist in equilibrium with excess of solute. The saturation concentration is a function of the temperature.
Fr.: solution de Schwarzschild
Briefly following Einstein's publication of → General Relativity, Karl Schwarzschild discovered this solution in 1916 (Sitzungsberichte der Königlich Preussischen Akademie der Wissenschaften zu Berlin, Phys.-Math. Klasse, 189); → Schwarzschild black hole.
Fr.: solution singulière, ~ particulière
small solar system body
jesm-e kucak-e râžmân-e xoršidi
Fr.: petit corps du système solaire
A term introduced by the → International Astronomical Union (August 2006) to name the → solar system bodies other than → planets and → dwarf planets. Small solar system bodies include → asteroids, → comets, and → meteoroids.
Fr.: jour solaire martien
The solar day on Mars, which has a mean period of 24 hours 39 minutes 35.244 seconds (based on SI units), about 2.7% longer than Earth's solar day. The Martian sidereal day, as measured with respect to the fixed stars, is 24h 37m 22.663s, as compared with 23h 56m 04.0905s for Earth.
Sol, from L. sol "sun," cognate with Pers. hur, → Sun.
Of or pertaining to the Sun.
Adjective from L. sol; → Sun.
Fr.: abondance solaire
Fr.: activité solaire
solar activity cycle
carxe-ye žirandegi-ye xoršid
Fr.: cycle d'activité solaire
Same as the → solar cycle.
Fr.: analogue du soleil
A member of a class of unevolved or slightly evolved → Population I disk stars with an → effective temperature, degree of evolution, → metallicity, and kinematic property not very different from those of the Sun. See also → solar-like star; → solar twin.
Fr.: antiapex solaire
Fr.: apex solaire
The point on the celestial sphere toward which the Sun is apparently moving relative to the → local standard of rest. Its position, in the constellation → Hercules, is approximately R.A. 18h, Dec. +30°, close to the star → Vega. The velocity of this motion is estimated to be about 19.4 km/sec (about 4. AU/year). As a result of this motion, stars seem to be converging toward a point in the opposite direction, the → solar antapex.
solar axial tilt
gerâ-ye âse-ye xoršid
Fr.: inclinaison de l'axe du Soleil
gâhšomâr-e xoršidi (#)
Fr.: calendrier solaire
A calendar based on the apparent yearly motion of the Sun on the → celestial sphere. The year is usually reckoned with respect to the → vernal equinox, approximately for example in the case of the → Gregorian calendar and accurately in the case of the → Iranian calendar.
pâypa-ye xoršidi (#)
Fr.: constante solaire
The amount of solar radiation in all wavelengths received per unit of time per unit of area on a theoretical surface perpendicular to the Sun's rays and at Earth's mean distance from the Sun. Its mean value is 1367.7 W m-2 or 1.37 × 106 erg sec-1 cm-2. In other words, the solar constant is the mean → solar irradiance on the outer atmosphere when the Sun and Earth are spaced at 1 → astronomical unit. See also: → solar luminosity.
hurtâj, tâj-e xoršid (#)
Fr.: couronne solaire
The outermost atmosphere of the Sun immediately above the → chromosphere, which can be seen during a total solar eclipse. It consists of hot (1-2 × 106 K), extremely tenuous gas (about 10-16 g cm-3) extending for millions of kilometer from the Sun's surface.
carxe-ye xoršidi (#)
Fr.: cycle solaire
The periodic variation in frequency or number of solar active events (→ sunspots, → prominences, → flares, and other solar activity) occurring with an interval of about 11 years. The solar cycle was discovered in 1843 by Samuel Heinrich Schwabe (1789-1875), a German apothecary and amateur astronomer, who after 17 years of observations noticed a periodic variation in the average number of sunspots seen from year to year on the solar disk. Solar cycle numbering goes back to the 18-th century, when the Cycle 1 peak occurred in 1760. Cycle 23 peaked in 2000, and the following Cycle 24 will reach its maximum in 2013.