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: 12992 Search : far
fuzz
  پرز   
porz (#)

Fr.: duvet, poils fins   

1) Loose, light, fibrous, or → fluffy matter.
2) A mass or coating of such matter.
3) (Of an image) A blur. (Dictionary.com).

Of unknown origin; cf. Du. voos "spongy, woolly."

Porz "short fuzzy ends of fibers on the surface of cloth, any downy coating," of unknown etymology.

fuzzification
  پرزوارش   
porzvâreš

Fr.: fuzzification   

The first step carried out in a → fuzzy logic system during which a → crisp set of → input data are gathered and converted to a → fuzzy set using fuzzy → linguistic variables, fuzzy linguistic terms, and → membership functions.

Verbal noun of → fuzzify; → -tion.

fuzzify
  پرزواریدن   
pozvâridan

Fr.: fuzzifier   

To convert a → crisp set to a → fuzzy set in a → fuzzy logic system.

fuzzy; → -fy.

fuzziness
  پرزواری   
porzvâri

Fr.:   

The state or condition of being → fuzzy.

fuzzy; → -ness.

fuzzy
  پرزوار   
porzvâr

Fr.: flou, crépu   

1) Of the nature of or resembling → fuzz.
2) Covered with fuzz.
3) Indistinct; → blurred (Dictionary.com).
See also: → fuzzy image, → fuzzy logic, → fuzzy set.

From → fuzz + -y adj. suffix, from O.E. -ig, cognate with L. -icus, → -ic.

Porzvâr "resembling fuzz," from porz, → fuzz, + -var, a suffix of possession, similarity, and aptitude (e.g., omidvâr, sezâvâr, sugvâr, šâhvâr, gušvâr), → -oid.

fuzzy image
  وینه‌ی ِ پرزوار، تصویر ِ ~   
vine-ye porzvâr, ~ tasvir-e

Fr.: image floue, ~ estompée   

Same as → blurred image.

fuzzy; → image.

fuzzy inference system
  راژمان ِ دربرد ِ پرزوار   
râžmân-e darbord-e porzvâr

Fr.:   

A way of → mapping an → input space to an → output space using → fuzzy logic. FIS uses a collection of fuzzy → membership functions and rules, instead of Boolean logic, to reason about data. Also called → fuzzy logic system.

fuzzy; → inference; → system.

fuzzy inferencing
  دربرد ِ پرزوار   
darbord-e porzvâr

Fr.:   

A process used in a → fuzzy logic system where the → truth value for the premise of each rule is computed and applied to the conclusion part of each rule. This results in one fuzzy set to be assigned to each output variable for each rule.

fuzzy; → inference.

fuzzy logic
  گوییک ِ پرزوار   
guyik-e porzvâr

Fr.: logic flou   

A mathematical logic that recognizes more than simple → true and → false → propositions. With fuzzy logic, propositions can be represented with degrees of truthfulness and falsehood. In this system, → truth values are → fuzzy sets without sharp boundaries (→ crisp set) in contrast with → classical logic. Fuzzy logic is applied to a wide range of problems including: industrial control, domestic goods, decision making, robotics, intelligent machines, and image processing in medicine.

fuzzy; → logic.

fuzzy logic system
  راژمان ِ گوییک ِ پرزوار   
râžmân-e guyik-e porzvâr

Fr.: système de logic flou   

An engineering system which uses → fuzzy logic. It generally consists of four main components: → fuzzification interface (fuzzifier), → fuzzy rule base, → fuzzy inferencing unit, and → defuzzification interface (difuzzifier). Also called → fuzzy inference system.

fuzzy; → logic; → system.

fuzzy rule base
  پایگاه ِ رزن ِ پرزوار   
pâygâh-e razan-e porzvâr

Fr.:   

A rule base in a → fuzzy logic system constructed to control the → output variable. A fuzzy rule is a simple if-then rule with a condition and a conclusion.

fuzzy; → rule; → base.

fuzzy set
  هنگرد ِ پرزوار   
hangard-e porzvâr

Fr.: ensemble flou   

A set of → truth values in → fuzzy logic that does not have sharp boundaries. Instead, set members have degrees of membership. If the value of 1 is assigned to objects entirely within the set and a 0 is assigned to objects outside of the set, then any object partially in the set will have a value between 0 and 1. This contrast with → crisp sets in → classical logic where members assume a precise value of 1 or 0. Fuzzy sets were first introduced by Lotfi A. Zadeh (1965) and defined as follows. Let X be a space of points, with a generic element of X denoted by x. Thus X = {x}. A fuzzy set A in X is characterized by a → membership function  fA(x) which associates with each point in X a real number in the interval [0,1], with the values of fA(x) at x representing the "grade of membership" of x in A. Thus, the nearer the value of fA(x) to unity, the higher the grade of membership of x in A. Generally, the intersection operations of fuzzy sets are the expansion of that operation on → nonfuzzy sets. In other words, operations on nonfuzzy sets are a particular case of operations on fuzzy sets.

fuzzy; → set.

G band
  باند ِ G   
bând-e G

Fr.: bande G   

A conspicuous band of molecular → CH (methylidine) at 4300 Å, which is present in the spectra of late-type G-K stars.

G refers to → G type stars in the spectra of which this feature is strong. → band.

g mode
  ترز ِ g، مُد ِ ~   
tarz-e g, mod-e ~

Fr.: mode g   

Waves trapped inside stars, whose restoring force is the → buoyancy. Same as → gravity mode. See also: → oscillation modes; → p mode; → f mode.

g referring to gravity; → mode.

G ring
  حلقه‌ی ِ G   
halqe-ye G

Fr.: anneau G   

The → Saturn's ring, with a width of 8,000 km, lying before the → F ring, at 164,000-172,000 km from the center of Saturn.

ring.

G star
  ستاره‌ی G   
setâre-ye G

Fr.: étoile G   

A member of a class of stars to which the Sun belongs. The G-type stars on the → main sequence have → surface temperatures of 5,300-6,000 K and therefore appear yellow in color. G type → giant stars (such as → Capella) are almost 100-500 K colder than the corresponding main sequence stars. G type → supergiants have temperatures of 4,500-5,500 K. The spectrum of early type G stars, such as the Sun (G2), is dominated by ionized lines of calcium (→ H and K lines, mainly) and neutral metals. In later type G stars the molecular bands of → CH molecules and → CN molecules become visible. The main sequence and giant stars have masses of ~ 1 solar mass, while the supergiants are of ~ 10 solar masses. The luminosities of G-type giants are almost 30-60 times greater than that of the Sun, whereas the supergiants are 10,000-30,000 times more luminous.

G, from the → Harvard classification; → star.

G type star
  ستاره‌ی ِ گونه‌ی ِ G   
setâre-ye gune-ye G

Fr.: étoile de type G   

A yellowish star whose surface temperature is about 6000 K and its spectrum is dominated by H and K lines of ionized calcium (Ca II 3968 Å and 3934 Å).

G from the alphabetical sequence of spectral types; → type; → star.

G-type asteroid
  سیارک ِ گونه‌ی ِ G   
sayyârak-e gune-ye G

Fr.: astéroïde de type G   

A relatively uncommon → carbonaceous carbonaceous asteroid whose spectrum contains a strong → ultraviolet  → absorption feature below 0.5 μm (→ Tholen classification). In the → SMASS classification it corresponds to the Cg and Chg types , depending on the presence or absence (respectively) of the absorption feature at 0.7 μm. The most remarkable "asteroid" in this type is → Ceres (now classified as a → dwarf planet).

type; → asteroid.

G-type star
  ستاره‌ی گونه‌ی ِ G   
setâre-ye gune-ye G

Fr.: étoile de type G   

Same as → G star.

G star; → type.

Gaia
  گایا   
Gaia (#)

Fr.: Gaia   

A → European Space Agency  → astrometry mission launched on 19 December 2013. Gaia's goal is to create the largest and most precise three-dimensional chart of the → Milky Way galaxy by providing unprecedented positional (position on the sky and distance to the Sun) and annual → proper motion measurements for about one billion stars in our Galaxy and throughout the → Local Group. Moreover, the third component of the velocity, the → radial velocity, will be obtained for all stars down to V = 17 mag. Similarly, multi-color photometry will be carried out on all stars down to V = 20 mag. Gaia will achieve the planned astrometric requirements by repeatedly measuring the positions of all objects down to V = 20 mag with final accuracies of about 20 microarcsec at 15 mag. It will provide distances accurate to 20% as far as the → Galactic Center. The satellite is expected to be launched in 2012 and be placed in a → Lissajous orbit around the Sun-Earth → Lagrangian point L2. Gaia is a much more advanced version of the → Hipparcos mission.

Initially, GAIA was the short for Global Astrometric Interferometer for Astrophysics. Although subsequently the interferometer option was abandoned, the acronym was maintained in lower case.

<< < -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 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 Cop Cor cor cor cos cos Cou cou cow cre cri cro cry cur cut Cyg dam dar dat de deb dec dec ded def deg del dem den dep des det dev dia dif dif dig dio Dir dis dis dis dis dis dis div don dou dow dro dur dwa dyn Dys ear ebb ecl edg egg Ein Ela ele ele ele ele ell eme emp enc eng ent epi equ equ Equ esc eth Eur eve 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 fro fuz gai Gal Gal gam gas Gau gen gen geo geo geo gia glo gol gra gra gra gra gre gri gui H I hai Ham har Hau hea hec hel hel her HES hie hig his hom hor hot Hub hum Huy hyd hyd hyl hyp ice ide ima imm imp imp inc ind ind ine inf inf Inf inh inn ins ins int int int int Int int int int inv ion iri irr iso iso iso Jea Jor jun K s Kep keV kin Kol lad Lam lan lar las lat lea leg len lev lig lik lin lin lin Lis lob loc log loo low lum lun lun Lym Mac Mag mag mag mag mag Mag mak map Mar mas mat Mau mea mea med Men mer Mes met met mho mic Mie Mil min mis MK mod mol mon moo mot mul mul mut nak Nas nat neb neg neu neu New New nip noi non non noo Nor nuc nuc nul nut obj obl obs occ oct off old one ope opp opt opt orb ord org Ori osc oth ove oxi P-w pal par par par par Pas pat pej per per per per per per pha Phi pho pho pho phy pin Pla pla pla pla pla plu poi pol pol pol poo pos pos pot pra pre pre pre pre pri pri pro pro pro pro pro Pro pro pse pul pur qua qua qua qua que rac rad rad rad rad rad rad ran rar ray rea rea rec rec red red ref ref reg rel rel rel ren res res res res ret rev Ric rig rin roc roo rot rot Rus Sac sal sat sca sca Sch sci Scu sec sec Sed sel Sel sen ser sex Sha she sho sid sig sil sim sin siz sle SMA SNR Sof sol sol sol sol sou Sou spa Sp spe spe spe sph spi Spi spr sta sta sta sta sta ste ste Ste sto str str sub sub sub suf sun sup sup sup sup sur swo syn sys tak Tay Tel ten ter tet the the the thi Tho thu tid tim toa top tot tra tra tra tra tri tri tro Tru tur twi Typ UBV ult unb uni uni Uni Unu ura uti val vap vec Vel ver Ver vie vir vis vis vol W-R war wav wav wea wei Whe Wid win WN4 Wol X-p Yal you zep zir > >>