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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<< < -es -iv -ti 21- a p abe abs abs acc acc acc act act ada adi ads aes Age Alb Alf ali all alp alt ama amp ana ang ang ann ano ant ant ape apo app app arc Arg ari art ass ast ast ast atm ato att Aur aut axi azi bac Bal Bar Bar Bay Bec Ber bet bic bij bin bio Bir bla Bla blu blu bol Boo bou bra Bre bro bug C r cal Cal can car Car Cas cat cau cel cen cer Cha cha Cha che cho cir cir cir Cla cli clo clu co- cod coh col col col com com com com com com com com Com con con con con con con con con con con con coo cop Cor cor cor cos cos Cou cou CP cre cri cro CSP cur cya Cyg dan dar dat de- deb dec dec dee def deg del dem den dep des det dev dia dif dif dih dip dir dis dis dis dis dis diu doc doo dou dow Dru dus dwa dyn Dys Ear ecc eco edi EHB Ein ela ele ele ele ele ell eme emp end Eng ent epi equ equ Era est eth Eur evi exa exc exe exi exp exp ext ext eye fac fal Far fed Fer fer fie fin fir fit fla flo flu fol for for Fou fra fre Fre ful fuz Gal gal Gal gam gas Gau gen gen geo geo geo gib glo gos gra gra gra gra Gre gri gui H I hal Ham har Haw hea hei hel Hel her het hie hig Hob hom Hor hot Hub hum Huy hyd hyd hyp hyp ico if ima imp imp in- inc Ind ind ine inf inf inf ini ins ins int int int int int int int int int inv ion iro ise iso iso Jab jet Jov Jur Kee Kep kil Kis kry Lag lam lan Lar lat law lea lem lep Li lig lim lin lin lin lit loc loc lon Lor low lum lun Lup Lym mac mag mag mag mag mag mai man Mar mas mas mat Max mea mec meg Mer Mer met met met mic mid mil Min Mir mix mod mod MOL mon mor mov mul mur N66 Nap nat nea neg Ner neu New New nic nod non non non nor nov nuc nul num O-t obl obs obt och off Ohm on- opa Oph opt opt ora orb ord Ori ort osc out ove ozo pal pan par par par par pat pec pen per per per per per Pfu pha pho pho pho phy pie pla Pla Pla pla pla Plo poi pol pol pol pol por pos pot pow pre pre pre pre pri pri pri pro pro pro pro Pro pro Pru pul pul Pyt qua qua qua qua quo rad rad rad rad rad rad ram Ran rat re- rea rec rec red red ref ref reg Reg rel rel rem rep res res res ret rev rho rif Rin Rob Rom rot rot rul S D Sai san Sat sca Sch Sch scr sec sec sec sei sel sem sep set sha she sho sid sig sil sim sin sit sky Slo sno sof sol sol sol sol sor sou spa spa spe spe spe sph spi spi spr SS sta sta sta sta ste ste ste Sto str str stu sub sub suc sun sup sup sup sup sur swe syn syn tad Tau tel ten ter tet the the the thi Tho thr tid tim Tit top tot tra tra tra tra tre tri Tro tru tur TW Typ U G ult unb und uni uni uns ura use val vap vec Vel Ven Ver Vie Vir vir vis vol W V war wav wav wea Wei Wez wid win WN3 Wol Wro Y d YOR zen zir > >>

Number of Results: 12974 Search : far
Dyson sphere
  سپهر ِ دایسون   
sepehr-e Dyson

Fr.: sphère de Dyson   

A hypothetical structure built around a → star by an advanced → civilization to utilize most or all of the → energy radiated by their star. The idea of such a sphere was first formalized and popularized by theoretical physicist Freeman Dyson in 1960, though it was originally put forward by a 1945 science fiction novel. Dyson assumed that the power needs of → intelligent civilizations never stops increasing. He also proposed that searching for the existence of such structures might lead to the discovery of advanced civilizations elsewhere in the Galaxy. Sometimes referred to as a → Dyson shell or → megastructure.

Freeman John Dyson (1923-). His article, entitled "Search for Artificial Stellar Sources of Infrared Radiation," appeared in the 1960 issue of Science, 131 (3414), 1667-1668; → sphere.

DZ white dwarf
  سفید‌کوتوله‌ی ِ DZ   
sefid kutule-ye DZ

Fr.: naine blanche DZ   

A → white dwarf whose spectrum shows metal lines only; no H or He.

D short for → dwarf; Z a convention; → white.

E corona
  تاج ِ E   
tâj-e E

Fr.: couronne E   

A part of the → solar corona defined by the → emission lines of hot gases. These emission lines include the so-called → forbidden lines of the strongly ionized atoms of iron, calcium, and other elements. The E corona is thinner than the → K corona and the → F corona (M.S.: SDE).

E indicating → emission; → corona.

E ring
  حلقه‌ی ِ E   
halqe-ye E

Fr.: anneau E   

The → Saturn's ring, with a width of 300,000 km, lying beyond the → G ring, at 180,000-480,000 km from the center of Saturn.

ring.

E-ELT
     
E-ELT

Fr.: E-ELT   

The world's largest → optical and → near infrared telescope, with a diameter of 42 m, to be built by the → European Southern Observatory (ESO). → First light is foreseen for 2018. The telescope has an innovative five-mirror design that includes advanced → adaptive optics to correct for the → atmospheric turbulence, giving exceptional → image quality. The → primary mirror will consist of almost 1000 hexagonal segments each 1.4 m across. The → secondary mirror will be 6 m in diameter. The E-ELT will collect 15 times more light than the largest optical telescopes operating today.
On 26 April 2010, the ESO Council selected Cerro Armazones as the baseline site for the E-ELT. Cerro Armazones is a mountain at an altitude of 3060 m in the central part of Chile's Atacama Desert, some 130 km south of the town of Antofagasta and about 20 km from Cerro Paranal, home of ESO → Very Large Telescope.

Short for the European Extremely Large Telescope

e-folding time
  زمان ِ e-تایی   
zamân-e e-tâyi

Fr.:   

The time within which the amplitude of an oscillation increases or decreases by a factor e (= 2.71828...).

From e the base of the natural, or Napierian, system of logarithms; folding, from -fold suffix meaning "of so many parts," or denoting multiplication by the number indicated by the stem or word to which the suffix is attached (as in twofold; manifold), from O.E. -feald, related to Ger. -falt; Gk. altos, -plos, -plus; → time.

Zamân, → time; e, as above; tâyi noun of multiplicative suffix, also "fold, plait, wrinkle; like, resembling."

e-mail
  پَیِل   
payel

Fr.: mél, courriel   

1) A system for sending → messages from one individual to another via telecommunications links between → computers or → terminals using dedicated → software.
2) A message sent by email (Dictionary.com).

From electronic, → electronic, + mail, from M.E. male, from O.Fr. male "wallet, bag," of Germanic source; cf. O.H.G. malaha "wallet, bag," M.Du. male "bag;") from PIE *molko- "skin, bag."

Payel, contraction of payâm-e elelktronik "electronic message," from payâm, → message, + elektronik, → electronic; cf. Fr. mél "e-mail," from message + électronique, or courriel "e-mail," from courrier + électronique.

E-mode polarization
  قطبش ِ ترز ِ E   
qotbeš-e tarz-e E

Fr.: polarisation en mode E   

A → polarization component in the → cosmic microwave background radiation that depends only on → gradient, is independent of → curl and does not have → handedness. In contrast to the → B-mode, the E-mode may be due to both the → scalar perturbations and → tensor perturbations.

E, indicating electric-field like; → mode; → polarization.

e-term of aberration
  بیراهش ِ ترم ِ e   
birâheš-e tarm-e e

Fr.: aberration elliptique   

The same as → elliptic aberration.

e, → elliptic; → term; → aberration.

E-type chondrite
  کوندریت ِ گونه‌ی ِ E   
kondrit-e gune-ye E

Fr.: chondrite de type E   

Same as → enstatite chondrite.

enstatite; → type; → chondrite.

Eagle Nebula (IC 4703)
  میغ ِ شاهین   
Miq-e Šâhin

Fr.: Nébuleuse de l'Aigle   

A prominent → H II region in the constellation → Serpens lying about 2 kpc away from the Sun. It measures about 30' across and surrounds the open cluster → M16 (NGC 6611), which contains at least 20 stars of spectral type B0.5 or earlier, including one 05V. At a projected distance from the cluster of about 2 pc, where the H II region has expanded into surrounding → molecular cloud, a striking → elephant trunk morphology or → pillar results. The nebula is the site of ongoing → star formation, especially in these pillar structures. The Eagle Nebula is often erroneously given the cluster's designation (M16).

Eagle, because the nebula's shape is vaguely reminiscent of an eagle in flight; from M.E. egle, from O.Fr. egle, from O.Prov. aigla, from L. → aquila "black eagle;" → nebula.

Miq, → nebula; Šâhin, → aquila.

ear
  گوش   
guš (#)

Fr.: oreille   

The vertebrate organ of hearing, which is also responsible for maintaining equilibrium. It is usually composed of three parts: the outer ear, middle ear, and inner ear.

M.E. ere, O.E. eare "ear" (O.N. eyra, Dan. øre, M.Du. ore, Du. oor, O.H.G. ora, Ger. Ohr); cf. Gk. aus; L. auris; Av. usi "both ears;" Lith. ausis; O.C.S. ucho; O.Ir. au; PIE *ous-.

Guš "ear" (gušidan "to hear," niyušidan "to listen"); Mid.Pers. gôš "ear," gôšidan "to hear, listen;" O.Pers. gauša-; Av. gaoša- "ear," gaoš- "to hear;" cf. Skt. ghosa- "noise, tumult," ghus- "to sound, cry or proclaim aloud;" PIE *ghous-.

early
  آغازین   
âqâzin (#)

Fr.: précoce; jeune   

Occurring at or near the beginning of a period of time, process, or sequence of events.

M.E. erlich (adj.), erliche (adv.); O.E. ærlice, from ær "soon, ere" (from P.Gmc. *airiz, from PIE *āier- "day, morning," cf. Av. ayar- "day, day time," ayarə.drājah- "duration of one day," ayarə.bara- "day's ride," Mid/Mod.Pers. parēr "the day before yesterday," from *parā.ayer- "the day before") + -lice "-ly," adverbial suffix.

Âqâzin adj. of âqâz "beginning," from Proto-Iranian *āgaHz-, from prefix ā- + *gaHz- "to run, start," cf. Sogdian āγāz "beginning, start" (Cheung 2007).

early AGB phase
  فاز ِ AGBی ِ آغازین   
fâz-e AGB-ye âqâzin

Fr.: phase initiale de l'AGB   

A fairly long-lived step in the evolution of → low-mass and → intermediate-mass stars when helium burning shifts from the center to a shell around the core. At this phase the stellar luminosity is provided almost entirely by → helium shell burning. The He-shell burning generally adds mass to the growing carbon/oxygen core, resulting in → degenerate matter due to its increasing density.

early; → AGB; → phase.

early solar system
  راژمان ِ خورشیدی ِ آغازین   
râžmân-e xoršidi-ye âqâzin

Fr.: système solaire primordial   

A period in the evolution of the → solar system when the planets and satellites were in the process of formation.

early; → solar; → system.

early spectral class star
  ستاره با رده‌ی ِ بینابی ِ آغازین   
setâré bâ rade-ye binâbi-ye âqâzin

Fr.: étoile de type spectral précoce   

A star near the beginning of the → spectral classification sequence. A star of → spectral type O, B, A, or F0 to F5. Same as → early-type star.

early; → spectral; → class; → star.

early Universe
  گیتی ِ آغازین   
giti-ye âqâzin (#)

Fr.: Univers jeune   

A qualitative term used to describe a phase in the history of the Universe, from the → Big Bang event to the apparition of the first structures (seeds of future galaxies), at a → redshift around 30.

early; → universe.

early-type galaxy (ETG)
  کهکشان ِ گونه‌ی ِ آغازین   
kahkešân-e gune-ye âqâzin

Fr.: galaxie de type précoce   

In the → Hubble classification, galaxies on the left part of the → Hubble sequence. Early-type galaxies tend to have redder colors, higher average surface brightnesses, and lower → neutral hydrogen content than → late-type galaxies. This terminology is based on the obsolete and erroneous idea that → elliptical and → lenticular galaxies might be evolutionary precursors to → spiral and → barred spiral galaxies.

early; → type; → galaxy.

early-type star
  ستاره‌ی ِ گونه‌ی ِ آغازین   
setâre-ye gun-ye âqâzin (#)

Fr.: étoile de type précoce   

Hot, luminous stars of → spectral type O, B, A, and F0 to F5. They were originally thought, wrongly, to be at an earlier stage of evolution than → late-type stars. See also → spectral classification.

early; → type; → star.

Earth
  زمین   
zamin (#)

Fr.: terre   

The third planet from the Sun. At → perihelion, it is 147,099,590 km from the Sun, and at → aphelion it is 152,096.150 km, whereas its mean distance from the Sun (→ astronomical unit) is 149,598 × 106 km. Its orbital period is 365.2563 days (→ sidereal year) and its → eccentricity 0.017. Other characteristics: → axial inclination 23.44°; rotation period 23.934 h (→ sidereal day); mean density 5.52 g/cm3; mass 5.974 × 1024 kg; → escape velocity 11.18 km/s; average → albedo 0.37.
The Earth's atmosphere consists of 78% nitrogen, 21% oxygen and 0.9% argon, plus carbon dioxide, hydrogen, and other gases in much smaller quantities. The atmospheric pressure at sea level is about 1,000 mbar. The surface average temperature is 15° C, but it varies, on the average, between -50° C (winter, Siberia) and up to + 40° C (summer, Sahara).
Liquid water covers 71% of the surface. Over 5,000 active volcanoes have been registered throughout man's known history. The outer layer of the planet, the → lithosphere, is covered with the → crust. In the → upper mantle and beneath the lithosphere, lies → asthenosphere. Convection in the asthenosphere has caused → plate tectonics motions and continent drifts. The densest layer of the Earth is its → core, about 3000 km to 6400 km beneath the surface, consisting primarily of iron and nickel. This core is believed to be at the origin of the magnetic field, which reaches about 3 × 10-5 tesla near the equator. It has only one natural satellite, the Moon (M.S.: SDE).

M.E. erthe, from O.E. eorðe "ground, soil, dry land;" cf. O.N. jörð, M.Du. eerde, O.H.G. erda, Goth. airþa; from PIE base *er-.

Zamin, variant zami "earth, floor, land," Mid.Pers. zamig, Av. zam- "the earth;" cf. Skt. ksam- "the ground, earth;" Gk. khthôn, khamai "on the ground;" L. homo "earthly being" (as in homo sapiens, homicide, humble, humus, exhume), humus "the earth;" O.Russ. zemi "land, earth;" PIE root *dh(e)ghom "earth".

<< < -es -iv -ti 21- a p abe abs abs acc acc acc act act ada adi ads aes Age Alb Alf ali all alp alt ama amp ana ang ang ann ano ant ant ape apo app app arc Arg ari art ass ast ast ast atm ato att Aur aut axi azi bac Bal Bar Bar Bay Bec Ber bet bic bij bin bio Bir bla Bla blu blu bol Boo bou bra Bre bro bug C r cal Cal can car Car Cas cat cau cel cen cer Cha cha Cha che cho cir cir cir Cla cli clo clu co- cod coh col col col com com com com com com com com Com con con con con con con con con con con con coo cop Cor cor cor cos cos Cou cou CP cre cri cro CSP cur cya Cyg dan dar dat de- deb dec dec dee def deg del dem den dep des det dev dia dif dif dih dip dir dis dis dis dis dis diu doc doo dou dow Dru dus dwa dyn Dys Ear ecc eco edi EHB Ein ela ele ele ele ele ell eme emp end Eng ent epi equ equ Era est eth Eur evi exa exc exe exi exp exp ext ext eye fac fal Far fed Fer fer fie fin fir fit fla flo flu fol for for Fou fra fre Fre ful fuz Gal gal Gal gam gas Gau gen gen geo geo geo gib glo gos gra gra gra gra Gre gri gui H I hal Ham har Haw hea hei hel Hel her het hie hig Hob hom Hor hot Hub hum Huy hyd hyd hyp hyp ico if ima imp imp in- inc Ind ind ine inf inf inf ini ins ins int int int int int int int int int inv ion iro ise iso iso Jab jet Jov Jur Kee Kep kil Kis kry Lag lam lan Lar lat law lea lem lep Li lig lim lin lin lin lit loc loc lon Lor low lum lun Lup Lym mac mag mag mag mag mag mai man Mar mas mas mat Max mea mec meg Mer Mer met met met mic mid mil Min Mir mix mod mod MOL mon mor mov mul mur N66 Nap nat nea neg Ner neu New New nic nod non non non nor nov nuc nul num O-t obl obs obt och off Ohm on- opa Oph opt opt ora orb ord Ori ort osc out ove ozo pal pan par par par par pat pec pen per per per per per Pfu pha pho pho pho phy pie pla Pla Pla pla pla Plo poi pol pol pol pol por pos pot pow pre pre pre pre pri pri pri pro pro pro pro Pro pro Pru pul pul Pyt qua qua qua qua quo rad rad rad rad rad rad ram Ran rat re- rea rec rec red red ref ref reg Reg rel rel rem rep res res res ret rev rho rif Rin Rob Rom rot rot rul S D Sai san Sat sca Sch Sch scr sec sec sec sei sel sem sep set sha she sho sid sig sil sim sin sit sky Slo sno sof sol sol sol sol sor sou spa spa spe spe spe sph spi spi spr SS sta sta sta sta ste ste ste Sto str str stu sub sub suc sun sup sup sup sup sur swe syn syn tad Tau tel ten ter tet the the the thi Tho thr tid tim Tit top tot tra tra tra tra tre tri Tro tru tur TW Typ U G ult unb und uni uni uns ura use val vap vec Vel Ven Ver Vie Vir vir vis vol W V war wav wav wea Wei Wez wid win WN3 Wol Wro Y d YOR zen zir > >>