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 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 > >>

Number of Results: 13116 Search : far
wide field
  بزرگ-میدان   
bozog-meydân

Fr.: grand champ   

A telescope → field of view which covers a relatively large → angular area on the sky.

wide; → field.

Wide-field Infrared Survey Explorer (WISE)
  پویشگر برا‌ی ِ بردید ِ بزرگ-میدان در فروسرخ   
puyešgar barâye bardid-e bozorg-meydân dar forusorx

Fr.: Explorateur pour l'étude grand champ dans l'infrarouge   

A → NASA infrared astronomical → space telescope launched in December 2009 to carry out an → all-sky survey from 3 to 22 → microns. With its 40-cm → telescope telescope and → infrared cameras, WISE aimed at a wide variety of studies ranging from the evolution of → protoplanetary disks to the history of → star formation in normal galaxies. In early October 2010, after completing its prime science mission, the spacecraft ran out of → coolant that keeps its instrumentation cold. However, two of its four infrared cameras remained operational. Hence, NASA extended the NEOWISE portion of the WISE mission by four months, with the primary purpose of hunting for more → asteroids and → comets, and to finish one complete scan of the main → asteroid belt. In August 2013, the WISE telescope's mission was extended for more three years to search for asteroids that could collide with Earth.

wide field; → infrared; → survey; → explorer.

width
  پهنا   
pahnâ (#)

Fr.: largeur   

An extent from side to side; breadth; wideness. → bandwidth; → beamwidth; → equivalent width; → slitwidth.

From wide, M.E., O.E. wid (cf. Du. wijd, O.H.G. wit, Ger. weit) + -th a suffix forming nouns of quality or condition, M.E. -th(e); O.E. -thu, -th.

Pahnâ, from pahn "wide, broad," from Mid.Pers. pah(a)n; Av. paθana- "broad, wide, spacious."

Wiedemann-Franz law
  قانون ِ ویدمن-فرانتس   
qânun-e Wiedemann-Franz

Fr.: loi Wiedemann-Franz   

For all metals the ratio of the → thermal conductivity, κ, to the → electrical conductivity, σ, is directly proportional to the absolute temperature: K/σ = (1/3)(πk/e)2T, where k is → Boltzmann's constant and e the electron's charge.

Named after the German physicists Gustav Heinrich Wiedemann (1826-1899) and Rudolph Franz (1826-1902); → law.

Wien's displacement law
  قانون ِ جا-به-جایی ِ وین   
qânun-e jâ-be-jâyi-ye Wien (#)

Fr.: loi du déplacement de Wien   

The wavelength corresponding to the maximum emissive power of a black body is inversely proportional to the absolute temperature of the body: λmax.T = 0.29 cm-deg. Wien's law explains why objects of different temperature emit spectra that peak at different wavelengths. Hotter objects emit most of their radiation at shorter wavelengths; hence they will appear to be bluer. Wien's law was an early attempt to describe the → blackbody radiation. The law closely approximated the true shape of the blackbody spectrum at short wavelengths, but ultimately failed because it relied solely on classical physics. It was superseded by → Planck's radiation law, which correctly describes the blackbody spectrum at all wavelengths.

After the German physicist Wilhelm Wien (1864-1928), who found the law in 1896. He was awarded the 1911 Nobel Prize in physics; → displacement; → law.

Wiener-Khinchin theorem
  فربین ِ وینر-خینچین   
farbin-e Wiener-Khinchin

Fr.: théorème de Wiener-Khintchine   

A theorem used in signal processing whereby the → spectral density of a random signal is the → Fourier transform of the corresponding → autocorrelation function. In other words, the autocorrelation function and the spectral density function constitute a → Fourier transform pair. The Wiener-Khinchin theorem allows one to estimate the spectral density function from the Fourier transform of the autocorrelation function, which is easier to handle. The theorem has an important application particularly in radio astronomy. The two following → Fourier integrals are called the Wiener-Khinchin relations: K(τ) = ∫ J(f)e-iωτdf and J(f) = ∫ K(τ)eiωτ (both summed over -∞ to +∞), where K(τ) is the autocorrelation function and J(f) is the spectral density.

Named after Norbert Wiener (1894-1964), American mathematician, who first published this theorem in 1930, and Aleksandr Khinchin (1894-1959), Russian mathematician, who did so independently in 1934; → theorem.

wild
  توسن   
towsan (#)

Fr.: sauvage   

Living in a state of nature; not tamed or domesticated (Dictionary.com).

M.E., from O.E. wilde; cognate with Du., O.H.G. wildi, Ger. wild, Sw. vild.

Towsan "wild," cf. Av. disav- "a kind of night predator animal."

wildlife
  زیست ِ توسن، توسن-زیست   
zist-e towsan, towsan-zist

Fr.: vie sauvage   

Animals and plants living in their natural habitat.

wild; → life.

Wilkinson Microwave Anisotropy Probe (WMAP)
     
WMAP

Fr.: WMAP   

A space telescope launched by NASA in 2001 which measures the temperature fluctuations in the → cosmic microwave background (CMB) radiation. It creates a full-sky map of the CMB, with a 13 arcminute resolution via multi-frequency observations. WMAP is the first mission to use a → Lagrangian point L2 as its permanent observing station at a distance of 1.5 million km. WMAP completed its prime two years of mission operations in September 2003 and is continuing in 2009 its observations for still several years to come. WMAP's measurements have played a considerable role in establishing the current standard model of cosmology. They are consistent with a Universe that is dominated by → dark energy, with negative pressure or a → cosmological constant. In this model, the age of the Universe is 13.73 ± 0.12 billion years. The current expansion rate of the Universe measured by the Hubble constant, is 70.5 ± 1.3 km·s-1 Mpc-1. The content of the Universe consists of 4.56% ± 0.15% ordinary → baryonic matter, 22.8% ± 1.3% → cold dark matter, and 72.6% ± 1.5% of → dark energy, that accelerates the → expansion of the Universe.

WMAP, short for Wilkinson Microwave Anisotropy Probe, in honor of David Todd Wilkinson (1935-2002), who had been a member of the mission's science team.

Wilson depression
  نشیب ِ ویلسون   
našib-e Wilson

Fr.: dépression de Wilson   

The depression on the → Sun's → photosphere associated with → sunspots and involving the → Wilson effect. The measured depression values vary between about 700 and 2,000 km.

Wilson effect; → depression.

Wilson effect
  اسکر ِ ویلسون   
oskar-e Wilson

Fr.: effet de Wilson   

A phenomenon in which the shape of → sunspots flattens as they approach the → Sun's limb due to the → solar rotation. More specifically, when a sunspot approaches the → solar limbs the width of the → penumbra, relative to the → umbra, on the side facing the center of the Sun seems to become narrower than on the side facing the limb. This phenomenon arises from a projection effect, and is due to a geometrical depression (the → Wilson depression) in the layers of constant → optical depth in sunspots (see, e.g., Sami K. Solanki, 2003, Sunspots: An overview, The Astron. Astrophys. Rev., 11, 153).

First noticed by Alexander Wilson (1714-1786); → effect.

Wilson-Bappu effect
  اسکر ِ ویلسون-باپو   
oskar-e Wilson-Bappu

Fr.: effet de Wilson-Bappu   

The strong correlation between the equivalent width of Ca II → H and K lines of a late-type giant or supergiant star with the absolute visual magnitude of the star.

O. C. Wilson & M. K. Vainu Bappu (1957, ApJ 125, 661); → effect.

WIMP
  ویمپ   
WIMP (#)

Fr.: WIMP   

A member of a broad class of hypothetical elementary particles moving with non-relativistical speeds at the time of structure formation in the early Universe. WIMPs have nonzero rest mass and participate only in the weak nuclear interaction. WIMPs are expected to have collapsed into a roughly isothermal, spherical halo within which the visible portion of our galaxy resides. → dark halo. The → neutralino, predicted by supersymmetric theories is the favorite WIMP candidate. Another candidate is the → axion. WIMPs are candidates for dark matter.

weak; → interction; → massive; → particle .

wind
  ۱) باد؛ ۲) پیچیدن   
1) bâd (#); 2) picidan

Fr.: 1) vent; 2) s'enrouler   

1a) Meteo.: Air in motion, especially a natural and perceptible movement of air relative to the ground.
1b) Astro.radiation-driven wind; → solar wind; → Galactic wind; → stellar wind.
2) To change direction; turn; to have a circular or spiral course or direction; to coil or twine about something.

1) M.E., O.E. wind (cf. O.S., O.Fris., Du. wind, O.H.G. wind, Ger. Wind, Goth. winds).
2) M.E. windan, from O.E. windan "to turn, twist, curl," cognate with Du. winden, O.H.G. wintan, Ger. winden, from PIE *wendh- "to turn, wind, weave."

1) Bâd, from Mid.Pers. wâd "wind;" Av. vāta- "wind;" cf. Skt. vāta- "wind, god of wind;" Gk. anemos "wind;" L. ventus "wind" (Fr. vent); cognate with E. wind, as above.
2) Picidan "to twist, entwine, coil," → spiral.

wind accretion
  فربال ِ بادی، ~ پت باد   
farbâl-e bâdi, ~ pat bâd

Fr.: accrétion par vent   

A quasi-spherical accretion that is likely to occur in a → high-mass X-ray binary (HMXB) when the optical star of → early spectral class (O-B) does not fill its → Roche lobe, but has a significant → mass loss via → stellar wind. In → close binary systems another accretion regime, → disk accretion, occurs when the optical star overfills its Roche lobe.

wind; → accretion.

wind blanketing
  پتومندی ِ باد   
patumandi-ye bâd

Fr.: effet de couverture du vent   

A process whereby dense winds of very luminous O type stars modify the temperature and internal structure of the underlying photosphere by scattering back a considerable part of the coming photospheric radiation. Not to be confused with → line blanketing .

Thus called because the wind acts like a blanket and heats the photosphere * by reflecting its radiation; → wind.

wind clumping
  گوده‌داری ِ باد   
gudedâri-ye bâd

Fr.: grumelage de vent   

The inhomogeneous property of a → radiation-driven wind, or the physical mechanism accounting for the → clumped wind.

clumpy; → wind.

wind luminosity
  تابندگی ِ باد   
tâbandegi-ye bâd

Fr.: luminosité de vent   

The final kinetic energy of the → stellar wind expressed by: (1/2)Mdot.v2 = (1/2)(v/c)L For an O6 star, L ~ 3 x 105Lsun and v ~ 2000 km s-1, which give a wind luminosity of ~ 1 x 1037 erg s-1, about 1% of the → stellar luminosity. See also → photon tiring limit.

wind; → luminosity.

wind momentum
  جنباک ِ باد   
jonbâk-e bâd

Fr.: moment angulaire de vent   

The product of the → mass loss rate and → terminal velocity used in the → radiation-driven wind theory. See also → modified wind momentum.

wind; → momentum.

wind rose
  بادنقش   
bâdnaqš (#)

Fr.: rose des vents   

A diagram showing the relative frequency of winds blowing from each of the 8 or 16 main points of the compass, sometimes within specified speed ranges, at a given location over a considerable period.

Translation of Ger. Windrose "compass card," from Windwind + Rose "rose," → Rosette Nebula.

Bâdnaqš, from bâd, → wind, + naqš "painting, engraving, printing," → map.

<< < -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 > >>