An Etymological Dictionary of Astronomy and Astrophysics
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فرهنگ ریشه شناختی اخترشناسی-اخترفیزیک

M. Heydari-Malayeri    -    Paris Observatory

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Number of Results: 13116 Search : far
electronic transition
  گذرش ِ الکترونی   
gozareš-e elektroni

Fr.: transition électronique   

The → transfer of an → electron from one → energy level to another.

electronic; → transition.

electronics
  الکترونیک   
elektronik (#)

Fr.: électronique   

The science dealing with the development and application of → devices and → systems involving the flow of → electrons in a → vacuum, in → gaseous media, and in → semiconductors (Dictionary.com).

electron; → -ics.

electroscope
  برق‌نما   
barqnemâ (#)

Fr.: électroscope   

An instrument for detecting electric charges or → potential differences.

electro-; → -scope.

electrostatic
  برق‌ایستا   
barqistâ

Fr.: électrostatique   

Referring to electric charges at rest.

electro-; → static.

electrostatic charge
  بار ِ برق‌ایستا   
bâr-e barqistâ

Fr.: charge électrostatique   

A quantity of electricity at rest on the surface of an insulator or an insulated conductor.

electrostatic; → charge.

electrostatic field
  میدان ِ برق‌ایستا   
meydân-e barqistâ (#)

Fr.: champ électrostatique   

A region of space in which a non-moving → electric charge would be subjected to a force of attraction or repulsion as a result of the presence of another stationary electric charge. The electrostatic field is a special case of the → electromagnetic field.

electrostatic; → field.

electrostatic induction
  درهازش ِ برق‌ایستا   
darhâzeš-e barqistâ

Fr.: induction électrostatique   

The production of stationary electric charges on an uncharged object as a result of a charged body being brought near it without touching it. A positive charge will induce a negative charge, and vice versa.

electrostatic; → induction.

electrostatic unit (esu)
  یکای ِ برق‌ایستای ِ بار   
yekâ-ye barqistâ-ye bâr

Fr.: unité électrostatique de charge   

The unit of electric charge in the → cgs system of units. Also called the → statcoulomb. The esu is defined such that if two objects, each carrying a charge of +1 esu, are 1 cm aparat, then they repel each other with a force of 1 → dyne. 1 esu = 3.3356 × 10-10 → coulombs.

electrostatic; → unit; → charge.

electrostatic wave
  موج ِ برق‌ایستا   
mowj-e barqistâ

Fr.: onde électrostatique   

In a → plasma, a disturbance that is devoid of magnetic field, and hence can be expressed by an electrostatic potential. The electric field is always parallel to the propagation vector, so that the electrostatic wave is → longitudinal.

electrostatic; → wave.

electrostatics
  برق‌ایستاییک   
barqistâyik

Fr.: électrostatique   

The branch of → electricity dealing with the phenomena and properties of stationary → electric charges, as opposed to → electrodynamics. It involves the build-up of charge on the → surface of → objects due to → contact with other surfaces.

electro- + → statics.

electroweak
  برقانزار   
barqânezâr

Fr.: électrofaible   

Of, relating to, or being the → unification of → electromagnetism and the → weak interaction.

electro-; → weak.

electroweak epoch
  زیمه‌ی ِ برقانزار   
zime-ye barqânezâr

Fr.: époque électrofaible   

A period in the early history of the Universe lasting from 10-36 to 10-12 seconds after the → Big Bang. The electroweak epoch begins at the same time as cosmic → inflation is triggered. This is also the time when the → strong force breaks from the → grand unified force and ends with another → phase transition will occur in which the → weak interaction breaks from the → electroweak force.

electroweak; → epoch.

electroweak force
  نیروی ِ برقا نزار، ~ برقا کمزور   
niru-ye barqânezâr, ~ barqâkamzur

Fr.: force électrofaible   

The force that takes part in an → electroweak interaction.

electroweak; → force.

electroweak interaction
  اندرژیرش ِ برقانزار   
andaržireš-e barqânezâr

Fr.: interaction électrofaible   

The unified description of two of the four fundamental interactions of nature, → electromagnetism and the → weak interaction which would merge into a single force under conditions of extreme temperature (above 1016 degrees, 102 GeV) prevalent in the early history of the → Universe.

electroweak; → interaction.

electroweak star
  ستاره‌ی ِ برقانزار   
setâre-ye barqânezâr

Fr.: étoile électrofaible   

A postulated type of star that could form toward the end of a → massive star's life, after → nuclear fusion has stopped in its → core, and before the star → collapses into a → black hole. In those → extreme conditions, when → temperature and → density inside the star are very high, → quarks could convert into → leptons. Hence huge amounts of energy can be released, much of which would be in the form of → neutrinos.

electroweak; → star.

elegance
  قشنگی   
qašangi (#)

Fr.: élégance   

Elegance quality; something elegant.

Noun from → elegant.

elegant
  قشنگ   
qašang (#)

Fr.: élégant   

Gracefully refined and dignified, as in tastes, habits, or literary style; graceful in form or movement; excellent; fine; superior (Dictionary.com).

M.E., from M.Fr., from L. elegantem (nominative elegans) "choice, fine, tasteful," from eligere "to select, choose."

Qašang "elegant, nicely fitted up" (Steingass), variant šang; cf. Sogd. xšang "beautiful, magnificient, excellent," maybe related to Av. xšnu- "to entertain, welcome, take care of (a guest)," O.Pers. xšnu- "to be satisfied, glad," Pers. xošnud "satisfied, content."

elegant equation
  هموگش ِ قشنگ   
hamugeš-e qašang

Fr.: équation élégante   

An equation with surprising simplicity that expresses a fundamental result relating several apparently unassociable elements. For example, → Euler's formula for the particular case of θ = π, and the → mass-energy relation.

elegant; → equation.

element
  بن‌پار، عنصر   
bonpâr (#), onsor (#)

Fr.: élément   

1) General: A component or constituent of a whole or one of the parts into which a whole may be resolved by analysis.
2) Astro.: Any of the data required to define the precise nature of an orbit and to determine the position of a planet in the orbit at any given time. → orbital element.
3) Chemistry:: One of the 117 presently known substances that cannot be decomposed by chemical reaction into a simpler substance.
4) Math.:a) Of a cylinder or cone, the generating line of the surface, taken in any position. b) Of a set, any member of the set.

From O.Fr. élément, from L. elementum "rudiment, one of the four elements, first principle," origin unknown.

Bonpâr, from bon "basis; root; foundation; bottom;" Mid.Pers. bun "root; foundation; beginning," Av. būna- "base, depth," cf. Skt. bundha-, budhná- "base, bottom," Pali bunda- "root of tree" + pâr contraction of pâré "piece, part, portion, fragment;" Mid.Pers. pârag "piece, part, portion; gift, offering, bribe;" Av. pāra- "debt," from par- "to remunerate, equalize; to condemn;" PIE *per- "to sell, hand over, distribute; to assign;" cf. L. pars "part, piece, side, share," portio "share, portion;" Gk. peprotai "it has been granted;" Skt. purti- "reward;" Hitt. pars-, parsiya- "to break, crumble." Onsor from Ar.

element diffusion
  پخش ِ بن‌پار   
paxš-e bonpâr

Fr.: diffusion des éléments   

An important physical process occurring in stars, which is the relative separation of the various → chemical elements. It is caused by → gravitational settling and → thermal diffusion, on the one hand, and → radiative levitation on the other. This process, which was described by Michaud (1970) to account for the abundance anomalies observed in → chemically peculiar  → A star, is now recognized as occuring in all types of stars. Its influence on the observed → chemical abundances is extremely variable, however, due to competing macroscopic motions like → convective  → mixing or rotation-induced → turbulence. In the Sun, no observable abundance anomalies are expected from element diffusion, as the time scale of the process is longer than the solar lifetime. However the small induced → depletion of → helium and → heavy elements by about 20% is detectable through → helioseismology. Such detections are more difficult in stars, as only global → oscillation modes can be detected, in contrast to the Sun, where local oscillations of the surface can be analyzed (Théado et al., 2005, A&A 437, 553).

element; → diffusion.

<< < -es -iv -ti 21 a p abe abs abs aca acc acc acr act ada adh Adr aer aga air Alf Alg alk Alp alt alu amm ana And ang ani ano ant ant Ap apo app app Aqu Arc arg arr asc ass ast ast asy atm ato att aur aut axi B-m bad Bal bar bar Bay Bed ber Bet bif bim bin bio bis bla ble blu Bod Bol bor bou Bra Bre bro bul C-t Cal Cam can car Car Cas cat cav cel cen cer Cha cha Cha che chl Cir cir cir Cla cli clo clu co- coc coh col col col Com com com com com com com com Com con con con con con con con con con con con con coo Cor Cor cor cos cos cos Cou cou Cra Cre cri cro cub cur cyc cyl Dan dat Dav de- Deb dec dec dee def deg del Den den der det deu dew dic dif dif dil Dip dir dis dis dis dis dis diu dod Dop dou Dra dua dus dwa dyn DZ Ear ecc eco edi EHB Ein ela ele ele ele ele ell eme emp end Eng ent epi equ equ era ESP eth Eur evi exa exc exe exi exp exp ext ext ext fac fal far fec Fer fer fie fin fir fis fla Flo flu fog for for Fou fra fre fre Fro fun G s Gal gal gal Gar gau geg gen geo geo geo ger gla gly gra gra gra gra gra Gre gro GYR Had Hal hap Har HD hea hel hel Hen Her hex hig Hil hol Hoo hor hou Hub hum hyb hyd hyd hyp hys ide ign ima imp imp in- inc Ind ind ine inf inf inf ini ins ins ins int int int int Int int int int inv ion iri irr iso iso iso Jea Jor jum K c Kep Ker kin kno lab Lam Lan Lap las lat Le lef len lev lig lig lin lin lin liq Lit loc log lon lou LS lun lun Lym M s Mag mag mag mag mag mag maj man Mar mas mas mat May mea mec mel mer mes met met met mic mid mil Min Mir mix mod mod mol mon mor mov mul mur mys nan nat nav nec Nep neu New New NGC nob nom non non nor nos nuc nuc num nut obj obl obs occ oct off oli oni ope opp opt opt orb ord org orp osc out ove oxi P-w pal par par par par Pas pat pej per per per per per per pha Phe pho pho pho phy pin pla Pla pla pla pla plu poi pol pol Pol pol por pos pot Poy pre pre pre pre pri pri pri pro pro pro pro pro pro Psa pul pum Q i qua qua qua qua R A rad rad rad rad rad rad Ram Ran rat rea rea rec rec red red ref ref reg rei rel rel rem rep res res res ret rev Rho Rie ril riv rog Ros rot rul S A Sag sam sat sca sca Sch Sco Sec sec sec seg sel sem sen set Sha sha shi sho sid sig sim sin Sir ske sli Smo soc sof sol sol sol sol sou sou spa spe spe Spe spe sph spi Spi spr sta sta sta sta sta ste ste ste Sto str str sub sub sub suc sun sup sup sup sup sur swa syn syn tac tas tel tem ter tes the the the the thi thr tid til tip ton tor tou tra tra tra tra Tri tri tru tsu tur two Typ UHE ult unc uni uni uni upg ura uti val var vec Vel ver Ver vie Vir vis vis vol W-R war wav wav wea Wei wha wid win WN3 Wol wri xen yok zen zij > >>