An Etymological Dictionary of Astronomy and Astrophysics

فرهنگ ریشه شناختی اخترشناسی-اخترفیزیک

M. Heydari-Malayeri    -    Paris Observatory



<< < -sc Sag sam sat sca Sch Sch scr sec sec SED sei sel sem seq Sex Sha she sho sid sil sim sin sit sky slu sno sof sol sol sol sol sou spa spa spe spe spe sph spi Spi spu sta sta sta sta ste ste ste sto Str str sub sub sub sug sup sup sup sup sur sus sym syn syz > >>

Number of Results: 1281
solar disk
  گرده‌ی ِ خورشید   
gerde-ye xoršid

Fr.: disque solaire   

The apparent shape of the → Sun's → photosphere.

solar; → disk.

solar dynamo
  توانزای ِ خورشیدی   
tavânzâ-ye xoršidi (#)

Fr.: dynamo solaire   

A model for explaining the generation of the → solar magnetic field and the related observational features (mainly → solar cycle, → Sporer's law, → Hale's law, → Joy's law, → polarity reversal). The global frame of this model is the interaction between a → turbulent plasma in the → convective zone (reciprocal generation of magnetic and electric fields) and the solar differential rotation (mutual transformation of meridional magnetic field into azimuthal magnetic field). The idea that a dynamo is responsible for generating the solar magnetic field was first proposed by Larmor (1919) and further developed by Cowling (1933), Parker (1955) and others.

solar; → dynamo.

solar eclipse
  خورگرفت، گرفت ِ خورشیدی   
xor gereft, gereft-e xoršidi (#)

Fr.: éclipse de soleil   

An eclipse in which the Earth passes through the shadow cast by the Moon. Solar eclipses only happen when the Moon is new and when the Moon lies close to the node of its orbit.

solar; → eclipse.

solar ecliptic limit
  حد ِ هورپهی ِ خورشید   
hadd-e hurpehi-ye xoršid

Fr.: limite écliptique du Soleil   

The greatest angular distance from a → lunar orbit node within which a → solar eclipse may occur when the Sun and Moon are in conjunction there. The solar ecliptic limit extends about 17° on each side of the node.

solar; → ecliptic; → limit.

solar equation
  هموگش ِ خورشیدی   
hamugeš-e xoršidi

Fr.: équation solaire   

In ancient astronomy, the difference between the Sun's mean and actual position. The ancients observed that, although the motion of the Sun in the ecliptic is almost uniform, it is subject to a small annual variation.

solar; → equation.

solar flare
  آلاو ِ خورشیدی   
âlâv-e xoršidi (#)

Fr.: éruption solaire   

A bright eruption form the Sun's → chromosphere in the vicinity of a → sunspot. Solar flares are caused by tremendous explosions on the surface of the Sun. In a matter of just a few minutes they heat the material to many millions of degrees and release as much energy as a billion → megatones of → T.N.T..

solar; → flare.

solar instrument
  سازال ِ خورشیدی   
sâzâl-e xoršidi

Fr.: instrument solaire   

An instrument especially designed for solar observations.

solar; → instrument.

solar irradiance
  تابشداری ِ خورشیدی   
tâbešdâri-ye xoršidi

Fr.: irradiation solaire   

The radiative power per unit area in all wavelengths from the Sun received by the Earth at its average distance from the Sun. Its mean value is called the → solar constant. The solar irradiance changes over a year by about 6.6% due to the variation in the Earth/Sun distance. Moreover, solar activity variations cause irradiance changes of up to 1%.

solar; → irradiance.

solar limb
  لبه‌ی ِ خورشید   
labe-ye xoršid

Fr.: bord solaire   

The edge of the → disk of the → Sun.

solar; → limb.

solar longitude
  درژنای ِ خورشیدی   
derežnâ-ye xoršidi

Fr.: longitude du Soleil   

The ecliptic longitude of the Sun. It varies from 0° (at the vernal equinox) to 360° during the year. By Kepler's Second Law, the rate of change of the solar longitude is such that the Earth sweeps out equal areas on the ecliptic plane in equal times.

solar; → longitude.

solar luminosity
  تابندگی ِ خورشید   
tâbandegi-ye xoršid (#)

Fr.: luminosité solaire   

The total → radiant energy, in all wavelengths, emitted by the Sun in all directions. It is 3.828 × 1026 W or 3.828 × 1033 erg sec-1 (International Astronomical Union, Resolution B3, 14 August 2015, Honolulu, USA). This is the luminosity unit conventionally used to give the luminosities of stars. See also: → solar constant.

solar; → luminosity.

solar magnetic cycle
  چرخه‌ی ِ مغناتیسی ِ خورشید   
carxe-ye meqnâtisi-ye xoršid

Fr.: cycle magnétique solaire   

The period of time, about 22 years, after which the magnetic → polarity of the Sun returns to its earlier state. It consists of two consecutive → solar cycles.

solar; → magnetic; → cycle.

solar magnetic field
  میدان ِ مغناتیسی ِ خورشید   
meydân-e meqnâtisi-ye xoršid (#)

Fr.: champ magnétique solaire   

The Sun's magnetic field which is probably created by the → differential rotation of the Sun together with the movement of charged particles in the → convective zone. Understanding how the solar magnetic field comes about is the fundamental problem of Solar Physics. The solar magnetic field is responsible for all solar magnetic phenomena, such as → sunspots, → solar flares, → coronal mass ejections, and the → solar wind. The solar magnetic fields are observed from the → Zeeman broadening of spectral lines, → polarization effects on radio emission, and from the channeling of charged particles into visible → coronal streamers. The strength of Sun's average magnetic field is 1 → gauss (twice the average field on the surface of Earth, around 0.5 gauss), and can be as strong as 4,000 Gauss in the neighborhood of a large sunspot.

solar; → magnetic; → field.

solar mass
  جرم ِ خورشید   
jerm-e xoršid (#)

Fr.: masse solaire   

The amount of mass in our Sun, 1.99 x 1033 g, about 330,000 times the Earth's mass. The solar mass is also the unit in which the masses of other stars, galaxies, and other large celestial bodies are expressed.

solar; → mass.

solar maximum
  بیشینه‌ی ِ خورشیدی   
bišine-ye xoršidi

Fr.: maximum solaire   

The month(s) during the 11 year → solar cycle when the number of → sunspots reaches a maximum.

solar; → maximum.

solar metallicity
  فلزیگی ِ خورشیدی   
felezigi-ye xoršidi

Fr.: métallicité solaire   

The proportion of the solar matter made up of → chemical elements heavier than → helium. It is denoted by Z, which represents the sum of all elements heavier than → helium, in mass fraction. The most recent determination of the solar Z gives a value of 0.0134 (Asplund et al. 2009, ARAA 47, 481), corresponding to the present-day photospheric composition.

solar; → metallicity.

solar minimum
  کمینه‌ی ِ خورشیدی   
kamine-ye xoršidi

Fr.: minimum solaire   

The month(s) during the 11 year → solar cycle when the number of → sunspots is lowest.

solar; → minimum.

solar nebula
  میغ ِ خورشیدی   
miq-e xoršidi

Fr.: nébuleuse solaire   

The cloud of interstellar gas and dust from which the Sun and the rest of the solar system initially formed.

solar; → nebula.

solar neighborhood
  همسایگی ِ خورشید   
hamsâyegi-ye xoršid (#)

Fr.: voisinage solaire   

That part of the Milky Way galaxy lying near the Sun. In fact there is no definition of the exact radius of this region. It is referred to the immediate solar neighborhood (within about 5 pc), the solar neighborhood (within about 25 pc), and the extended solar neighborhood (within a few hundred pc).

solar; → neighborhood.

solar neutrino
  نوترینوی ِ خورشیدی   
notinohâ-ye xoršidi

Fr.: flux des neutrinos solaires   

A neutrino generated in the → Sun. The main source of solar neutrinos is the → proton-proton chain of reactions: 4 × p→ He + 2e+ + 2νe, in which an energy of +28 MeV is shared between the reaction products. These are called → low-energy neutrinos. There are less important reactions in the Sun yielding a smaller flux of higher energy neutrinos. The solar neutrino flux can be estimated from the → solar luminosity (L), as follows Since there are two neutrinos for each 28 MeV of energy, the neutrino flux at the Earth distance (d) is given by: ν flux = 2Lsun/(28 MeV) × (1/4πd2) = 6 × 1010 cm-2 s-1. See also the → solar neutrino problem.

solar; → neutrino; → flux.

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