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
cosine
  کوسینوس   
kosinus (#)

Fr.: cosinus   

A trigonometric function giving the ratio of the side adjacent to a given angle to the hypotenuse.

Mod.L. complementi sinus, → com-; → sine.

cosmic
  کیهانی   
keyhâni (#)

Fr.: cosmique   

Of or relating to the → Universe (instead of universal which may lend to confusion), to the → outer space.

Adj. from → cosmos

cosmic acceleration
  شتاب ِ کیهانی   
šetâb-e keyhâni

Fr.: accélération cosmique   

accelerating Universe.

cosmic; → acceleration.

Cosmic Background Explorer (COBE)
  پویشگر ِ زمینه‌ی ِ کیهانی   
puyešgar-e zamin-ye keyhâni

Fr.: Satellite COBE   

NASA's satellite, designed to measure the diffuse infrared and → cosmic microwave background radiation from the early → Universe. It was launched on November 18, 1989 and carried three instruments: DIRBE (the Diffuse InfraRed Experiment), DMR (Differential Microwave Radiometers), and FIRAS (Far-InfraRed Absolute Spectrophotometer). The COBE observations showed that the cosmic microwave background spectrum matches that of a → blackbody of temperature 2.725 ± 0.002 K. COBE also found anisotropies in the cosmic microwave background at a level of a part in 100,000 (→ cosmic microwave background anisotropy). These tiny variations in the intensity of the CMB over the sky show how matter and energy was distributed when the Universe was still very young. Later, through a process still poorly understood, the early structures developed into galaxies, galaxy clusters, and the large scale structure that we see in the Universe today. Two of COBE's principal investigators, George Smoot and John Mather, received the Nobel Prize in Physics in 2006 for their work on the project.

cosmic; → background; → explorer.

cosmic background radiation
  تابش ِ پس‌زمینه‌ی ِ کیهانی   
tâbeš-e paszaminé-ye keyhâni

Fr.: rayonnement du fond cosmique   

cosmic microwave background radiation (CMBR).

cosmic; → background; → radiation.

Cosmic Dark Age
  عصر ِ تاریک ِ کیهانی   
asr-e târik-e keyhâni

Fr.: âge sombre cosmique   

The period of time in the early history of the Universe, between the → recombination era and the advent of the → first stars.

cosmic; → dark; → age.

cosmic defect
  آک ِ کیهانی   
âk-e keyhâni

Fr.: défaut cosmique   

Topological irregularities in the → space-time  → continuum, caused by the abrupt cooling of the → early Universe shortly after the → Big Bang, as predicted by some → cosmological models. These regions of immensely high density might have been the seeds of → structure formation through → gravity. Same as → topological defect.

cosmic; → defect.

cosmic distance scale
  مرپل ِ دورای ِ کیهانی   
marpel-e durâ-ye keyhâni

Fr.: échelle des distances cosmiques   

Measurement of the distances to the farthest objects in the Universe based on a bootstrapping series of methods, each applicable to more distant objects, and each dependent on the previous methods.

cosmic; → distance; → scale.

cosmic dust
  غبار ِ کیهانی، گرد ِ ~   
qobâr-e keyhâni (#), gard-e ~ (#)

Fr.: poussière cosmique   

Aggregations of matter on the order of a fraction of a micron across, irregularly shaped, and composed of → carbon and/or → silicates found in the → interstellar medium. Dust absorbs stellar light causing large dark patches in regions of the → Milky Way Galaxy and dark bands across other galaxies.

cosmic; → dust.

cosmic energy equation
  هموگش ِ کاروژ ِ کیهانی   
hamugeš-e kâruž-e keyhâni

Fr.: équation de l'énergie cosmique   

Same as the → Layzer-Irvine equation.

cosmic; → energy; → equation.

cosmic expansion
  سپانش ِ کیهانی   
sopâneš-e keyhâni

Fr.: expansion cosmique   

Same as the → expansion of the Universe.

cosmic; → expansion.

cosmic Eyelash (SMM J2135-0102)
  مژه‌ی ِ کیهانی   
može-ye keyhâni

Fr.: Cil cosmique   

A galaxy at a → redshift of z = 2.3259 lying behind a massive → cluster of galaxies and magnified by the → lensing effect of the cluster. It was first discovered in → submillimeter waves. The lensing cluster lies at a redshift z > 1.5 causing an → amplification factor for the background galaxy of 32 (A. M. Swinbank et al. 2010, Nature 464, 733).

cosmic; eyelash, from → eye + lash, from M.E. lashe (n.) lashen (v.) "to blow, stroke." Such called because of its narrow and elongated shape.

Možé "eyelash," from Mid.Pers. mec "eyelash," mecitan "to blink;" cf. Skt. mes "to open the eyes;" O.C.S. po-mežiti "to close the eyes;" keyhâni, → cosmic.

cosmic filament
  رشته‌ی ِ کیهانی   
rešte-ye keyhâni

Fr.: filament cosmique   

A very large-scale structure made of → galaxy clusters threaded like beads on a chain. Cosmic filaments are chiefly made up of → dark matter but also, to a lesser extent, of → baryonic matter. They are the largest entities in the → Universe and can be up to 1 billion → light-years long. They are separated by great → voids.

cosmic; → filament.

cosmic horizon
  افق ِ کیهانی   
ofoq-e keyhâni (#)

Fr.: horizon cosmologique   

The → observable region of the → Universe, limited in extent by the distance → light has traveled during the time elapsed since the beginning of the Universe (→ Big Bang). No signal from the objects lying beyond the cosmic horizon can be received because light has not yet had enough time to travel the distance. The cosmic horizon can be defined in two ways:
1) The size of the → observable Universe as derived from ct, where c is the → speed of light and t is the → age of the Universe, 13.8 billion years, hence 13.8 billion → light-years.
2) The → comoving distance. The distance given above corresponds to the size Universe had 13.8 billion years ago. Since then the Universe has been growing at a rate of 3.52c. Therefore, the current radius of the observable Universe is about 48 × 109 light-years. Same as → particle horizon, → Hubble distance, → Hubble radius, and → Hubble length. See also → sound horizon.

cosmic; → horizon.

cosmic infrared background (CIB)
  پس‌زمینه‌ی ِ فروسرخ ِ کیهانی   
paszamine-ye forusorx-e keyhâni

Fr.: le cosmique infrarouge   

A diffuse radiation which consists of the cumulative infrared emission from all galaxies throughout cosmic history. It is about 50 times weaker than the → cosmic microwave background radiation (CMBR). Since the CIB is produced by the dust within such galaxies, it carries a wealth of information about the processes of star formation therein.

cosmic; → infrared; → background.

cosmic microwave background anisotropy
  ناهمسانگردیِ تابشِ ریزموجِ پس‌زمینه‌یِ کیهانی   
nâhamsângardi-ye tâbeš-e rizmowj-e paszaminé-ye keyhâni

Fr.: anisotropies du rayonnement du fond cosmique microonde   

Tiny fluctuations in the intensity of the → cosmic microwave background radiation (CMBR) as a function of angular position over the sky, first discovered in the → Cosmic Background Explorer (COBE) observations. At a level of 1 part in 100,000, these temperature variations trace the distribution of matter and energy when the Universe was very young, about 380,000 years old. Since the CMB spectrum is described to a high precision by a → blackbody law with temperature T0, it is usual to express the anisotropies in terms of temperature fluctuations ΔT/T0 and expand them on the sky in → spherical harmonic series ΔT/T0 (θ,φ) = Σ almYlm(θ,φ), where θ and φ are the → spherical polar coordinates, Ylm is the spherical harmonic functions with → multipole index l, and the sum runs over l = 1, 2, ..., ∞, m = -l, ..., l, giving 2l + 1 values of m for each l, and alm is the multipole moment of the decomposition. The power spectrum of the anisotropies is defined as Cl≡ mean | alm |2 = 1/(2l + 1) Σ mean | alm |2. See also → CMB angular power spectrum.

cosmic; → microwave; → background; → anisotropy.

cosmic microwave background polarization
  قطبش ِ زمینه‌ی ِ ریزموج ِ کیهانی   
qotbeš-e zamine-ye rizmowj-e keyhâni

Fr.: polarisation du rayonnement du fond cosmique microonde   

The polarization of the → cosmic microwave background radiation due to → Thomson scattering by → free electrons during the → recombination era. The polarization can greatly enhance the precision with which the parameters associated with → acoustic oscillations are derived; because it carries directional information on the sky. When an → electromagnetic wave is incident on a free electron, the scattered wave is polarized perpendicular to the incidence direction. If the incident radiation were → isotropic or had only a → dipole variation, the scattered radiation would have no net polarization. However, if the incident radiation from perpendicular directions (separated by 90°) had different intensities, a net → linear polarization would result. Such → anisotropy is called → quadrupole because the poles of anisotropy are 360°/4 = 90° apart.

cosmic; → microwave; → background; → polarization.

cosmic microwave background radiation (CMBR)
  تابشِ ریزموجِ پس‌زمینه‌یِ کیهانی   
tâbeš-e rizmowj-e paszaminé-ye keyhâni

Fr.: rayonnement du fond cosmique microonde   

The diffuse → electromagnetic radiation in the → microwave band, coming from all directions in the sky, which consists of relic photons left over from the very hot, early phase of the → Big Bang. More specifically, the CMBR belong to the → recombination era, when the → Universe was about 380,000 years old and had a temperature of about 3,000 K, or a → redshift of about 1,100. The photons that last scattered at this epoch have now cooled down to a temperature of 2.73 K. They have a pure → blackbody spectrum as they were at → thermal equilibrium before → decoupling. The CMB was discovered serendipitously in 1965 by Penzias and Wilson (ApJ L 142, 419) and was immediately interpreted as a relic radiation of the Big Bang by Dicke et al. (1965, ApJL 142, 383). Such a radiation had been predicted before by Gamow (1948, Nature 162, 680) and by Alpher and Herman (1948, Nature 162, 774). This discovery was a major argument in favor of the Big Bang theory. In 1992, the satellite → Cosmic Background Explorer (COBE) discovered the first anisotropies in the temperature of the CMB with an amplitude of about 30 µK. See also: → cosmic microwave background anisotropy, → dipole anisotropy, → CMB lensing, → CMB angular power spectrum, → acoustic peak, → baryon acoustic oscillation, → WMAP.

cosmic; → microwave; → background; → radiation.

cosmic neutrino background (CNB)
  نوترینو‌ی ِ پس‌زمینه‌ی ِ کیهانی   
notrino-ye paszamine-ye keyhâni

Fr.: fond cosmologique de neutrinos   

The theoretical → low-energy neutrinos that decoupled from the rest of matter about two seconds after the → Big Bang when the temperature dropped to approximately 2.5 MeV (redshift of z ~ 6 ×109). The CNB is similar to the → cosmic microwave background (CMB), but older. It is estimated that today the CNB has a temperature of Tν = (4/11)1/3Tγ, ~ 1.95 K (or 1.67 × 10-4 eV), where Tγ is the CMB temperature of 2.728 K. Also called the relic neutrinos.

cosmic; → neutrino; → background.

cosmic radio noise
  نوفه‌یِ رادیوییِ کیهانی   
nufe-ye râdioyi-ye keyhâni

Fr.: bruit radio cosmique   

Radio waves emanating from extraterrestrial sources.

cosmic; → radio; → noise.

<< < -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 > >>