An Etymological Dictionary of Astronomy and Astrophysics
English-French-Persian

فرهنگ ریشه شناختی اخترشناسی-اخترفیزیک

M. Heydari-Malayeri    -    Paris Observatory

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Number of Results: 13176 Search : far
hierarchical triple system
  راژمان ِ بستایی ِ ناپایگانی   
râžmân-e bastâyi-ye nâpâygâni

Fr.: système multiple non hiérarchique   

A triple star system in which the (inner) binary is orbited by a third body in a much wider orbit. → hierarchical multiple system.

hierarchical; → stellar; → system.

hierarchy
  پایگان   
pâygân (#)

Fr.: hiérarchie   

A system in which the components are organized in increasingly larger structures.

From O.Fr. ierarchie, from M.L. hierarchia "ranked division of angels," from Gk. hierarchia "rule of a high priest," from hierarches "high priest, leader of sacred rites," from ta hiera "the sacred rites" (neut. pl. of hieros "sacred") + archein "to lead, rule."

Pâygân, from pâyé "step, rank, degree," from pây, pâ "foot, step," from Mid.Pers. pâd, pây; Av. pad- "foot" (cf. Skt. pat; Gk. pos, gen. podos; L. pes, gen. pedis; P.Gmc. *fot; E. foot; Ger. Fuss; Fr. pied; PIE *pod-/*ped-) + -gân suffix forming plural entities, from Mid.Pers. -gânag, -gâna, from Proto-Iranian *kāna-ka-.

Higgs boson
  بوسون ِ هیگز   
boson-e Higgs (#)

Fr.: boson de Higgs   

A hypothetical, neutral → elementary particle which plays a key role in the → standard model of → particle physics. This massive particle, whose mass is estimated to be about 125 GeV (→ giga → electron-volts) and a zero → spin, carries the → Higgs field. In the current version of the → electroweak theory, → W boson and → Z boson and all the fundamental constituents (→ quarks and → leptons) get their masses by interacting with the Higgs boson. The Higgs boson is produced by the fusion of two → gluons via a triangular loop of virtual top quarks. In the decay process, a loop of virtual top quarks allows the Higgs boson to decay into two photons. The particle's discovery was announced by → CERN in July 2012.

Named after the Scottish physicist Peter Ware Higgs (1929-), one of the researchers who theorized the existence of this particle in 1964. In fact three groups of physicists almost simultaneously published their results on this subject: François Englert and Robert Brout in August 1964; Peter Higgs in October 1964; and Gerald Guralnik, Carl Hagen, and Tom Kibble in November 1964; → boson.

Higgs field
  میدان ِ هیگز   
meydân-e Higgs

Fr.: champ de Higgs   

A → scalar field supposed to be responsible for the genesis of → inertial mass. According to the → standard model of → particle physics, the Higgs field appeared 10-36 to 10-12 seconds after the → Big Bang, during the → electroweak epoch, when the temperature dropped below a critical threshold. The Higgs field permeates all space, and through its interaction with the fundamental particles it provides those particles with a mass. Any particle that does not interact with the Higgs field, such as the → photon, will be mass-less.

Higgs boson; → field.

Higgs mechanism
  ساز-و-کار ِ هیگز   
sâzokâr-e Higgs

Fr.: mécanisme de Higgs   

In the → standard model of → particle physics, a mechanism postulated to endow mass to → elementary particles. Simply put, a background field, called the → Higgs field, becomes locally distorted whenever a particle moves through it. The distortion generates the particle's mass.

Higgs boson; → mechanism.

high
  بلند؛ مِه؛ پُر   
boland (#); meh (#); por (#)

Fr.: haut   

1) Situated above the ground or exceeding the common degree or measure.
2) Exceeding the common degree or measure; strong; intense.
3) Meteo.: An area of high pressure, referring to a maximum of atmospheric pressure. Same as → anticyclone (Fr. haute pression).

M.E. heigh, variants hegh, hey, heh; O.E. heh, heah "of great height, lofty, tall," (cf. Du. hoog, O.H.G. hoh, Ger. hoch, Goth. hauhs "high;" also Ger. Hügel "hill"); from PIE *koukos "hill."

Boland "high," variants bâlâ "up, above, high, elevated, height," borz "height, magnitude" (it occurs also in the name of the mountain chain Alborz), Lori dialect berg "hill, mountain;" Mid.Pers. buland "high;" O.Pers. baršan- "height;" Av. barəz- "high, mount," barezan- "height;" cf. Skt. bhrant- "high;" L. fortis "strong" (Fr. & E. force); O.E. burg, burh "castle, fortified place," from P.Gmc. *burgs "fortress;" Ger. Burg "castle," Goth. baurgs "city," E. burg, borough, Fr. bourgeois, bourgeoisie, faubourg); PIE base *bhergh- "high."
Meh "great, large" (Mid.Pers. meh, mas, Av. maz-, masan-, mazant- "great, important," mazan- "greatness, majesty," mazišta- "greatest," cf. Skt. mah-, mahant-, Gk. megas, L. magnus; PIE *meg- "great").
Por "much, very, too much; full" (Mid.Pers. purr "full;" O.Pers. paru- "much, many;" Av. parav-, pauru-, pouru-, from par- "to fill;" PIE base *pelu- "full," from *pel- "to be full;" cf. Skt. puru-; Gk. polus; O.E. full).

High Accuracy Radial velocity Planet Searcher (HARPS)
  هارپس   
HARPS

Fr.: HARPS   

A high-precision echelle spectrograph built for exoplanet findings and installed on the ESO's 3.6m telescope at La Silla Observatory in Chile. The first light was achieved in February 2003. HARPS has discovered dozens of exoplanets, making it the most successful planet finder behind the Kepler space observatory. HARPS can detect movements as small as 0.97 m s-1 (3.5 km h-1), with an effective precision of the order of 30 cm s-1, and a → resolving power of 120,000 (Mayor et al., 2003, ESO Messengar 114, 20).

high; → accuracy; → radial; → velocity; → planet; → search; → -er.

High Energy Stereoscopic System (H.E.S.S.)
  راژمان ِ استریوی ِ مه‌ کاروژ   
râžmân-e estereyo-ye meh kâruž (H.E.S.S.)

Fr.: Système stéréoscopique de haute énergie (H.E.S.S.)   

An array of → IACT telescopes for studying cosmic → gamma rays in the 100 GeV to 100 TeV energy range. The HESS observatory is located in Namibia, southern Africa, at an altitude of 1800 m, and the project is an international collaboration of more than 100 scientists from nine countries. In its Phase I, HESS used four telescopes each consisting of a light collector with a diameter of 13 m and a focal length of 15 m placed at the corners of a square 120 m apart. Each telescope is segmented into 380 round mirror facets of 60 cm diameter and uses a camera consisting of 960 closely packed → photomultiplier tubes. The first of the telescopes went into operation in Summer 2002. Phase II includes a fifth telescope, called Large Cherenkov Telescope (LCT), of 27 m diameter, located in the centre of the initial array. This upgrade lowers the triggering threshold of the HESS array to about 20 GeV, thus broadening the energy window in which gamma-ray astronomy can be done, opening up more opportunities in astrophysical research (see, e.g., Bernlöhr et al. 2003, Astroparticle Physics 20, 111).

H.E.S.S., short for High Energy Stereoscopic System, is also intended to pay homage to Victor F. Hess (1883-1964), an Austrian-American physicist who received the Nobel Prize in Physics in 1936 for his discovery of → cosmic rays.

high latitudes
  وَروناهای ِ بالا   
varunâhâ-ye bâlâ

Fr.: hautes latitudes   

The latitude belt roughly between 60 and 90 degrees North and South. Also referred to as the polar region.

high; → latitude.

high redshift object
  بر‌آخت ِ مه-سرخ‌کیب   
barâxt-e meh-sorxkib

Fr.: objet à grand décalage vers le rouge   

A galaxy or quasar having a → redshift larger than about 0.8, corresponding to a → look-back time half the present age of the Universe. The qualifier "high" is, however, relative and depends on context and authors' assessment.

high; → redshift; → object.

high tide
  اوپیش، کشند، مد   
owpiš (#), kešand (#), madd (#)

Fr.: marée haute   

The state of the → tide when at its highest level.

high; → tide.

Owpiš, from Persian Gulf dialects, literally "forward water," from ow, variant of âb, → water, + piš "→ forward."
Madd, loan from Ar.

high water
  اوپیش، برکشند، مد   
owpiš (#), barkešand (#), madd(#)

Fr.: marée haute   

Also known as → high tide.

high; → water.

high-energy astrophysics
  اخترفیزیک ِ مه‌کاروژ   
axtarfizik-e meh-kâruž

Fr.: astrophysique des hautes énergies   

A branch of astrophysics that deals with objects emitting highly energetic radiation, such as X-ray astronomy, gamma-ray astronomy, and extreme ultraviolet astronomy, as well as neutrinos and cosmic rays.

high; → energy; → astrophysics.

high-energy cosmic rays
  پرتوهای ِ کیهانی ِ مه‌کاروژ، ~ ~ پرکاروژ   
partowhâ-ye keyhâni-ye meh-kâruž, ~ ~ por-kâruž

Fr.: rayons cosmiques de hautes énergies   

Cosmic rays which typically have energies in the range 1015 to 1020 electron volts. For the most part, they are protons and other atomic nuclei, and come from distant cosmos, perhaps even from outside our own Galaxy.

high; → energy; → cosmic; → ray.

high-energy neutrino
  نوترینو‌ی ِ مه‌کاروژ   
notrino-ye meh-kâruž

Fr.: neutrino haute énergie   

A neutrino produced in high-energy particle collisions, such as those occurring when → cosmic rays strike atoms in the Earth's → atmosphere. Their energy range expands from a few → MeVs up to tenths of a → peta- (P) → electron-volts.

high; → energy; → neutrino.

high-excitation blob (HEB)
  ژیگ ِ پر-بر‌انگیزش   
žig-e por-barangizeš

Fr.:   

A rare class of → H II regions in the → Magellanic Clouds. In contrast to the typical H II regions of the Magellanic Clouds, which are extended structures (sizes of several arc minutes corresponding to more than 50 pc, powered by a large number of exciting stars), HEBs are very dense and small regions (~ 4" to 10" in diameter corresponding to ~ 1-3 pc). They have a higher degree of → excitation ([O III] 5007Å /Hβ) with respect to the typical H II regions, and are, in general, heavily affected by local → dust. They are powered by a relatively smaller number of → massive stars.

high; → excitation; → blob.

high-mass star
  ستاره‌ی ِ مِه‌جرم، ~ پُرجرم   
setâre-ye meh-jerm (#), ~ por-jerm (#)

Fr.: étoile massive   

A star whose mass exceeds 8 solar masses. Same as → massive star. → intermediate-mass star; → low-mass star.

high; → mass; → star.

high-mass X-ray binary (HMXB)
  درین ِ پرتو ایکس ِ پرجرم   
dorin-e partow-e iks-e por-jerm

Fr.: binaire X de forte masse   

A member of one of the two main classes of → X-ray binary systems where one of the components is a neutron star or a black hole and the other one a → massive star. HMXBs emit relatively → hard X-rays and usually show regular pulsations, no X-ray bursts, and often X-ray eclipses. Their X-ray luminosity is much larger than their optical luminosity. In our Galaxy HMXBs are found predominantly in the → spiral arms and within the → Galactic disk in young → stellar populations less than 107 years old. One of the most famous HMXB is Cygnus X-1 which was the first stellar-mass black hole discovered. See also: → low-mass X-ray binary.

high; → mass; → X-ray; → binary.

high-power laser
  لیزر ِ پُرتوان   
leyzer-e por-tavân (#)

Fr.: laser de puissance   

A laser beam with the output power in the range 1012-1015 watts/cm2, capable of depositing kilo-joule order energies during nano-second time intervals in small volumes (about 1 mm3). High power lasers, which can produce temperatures of 10-50 million degrees and pressures of 10-100 million bars, are used to simulate astrophysical conditions in laboratories.

high; → power;, → laser.

leyzer, → laser; por "much, many, full," → full; tavân, → power.

high-resolution observation
  نپاهش ِ مه-واگشود   
nepâheš-e mehvâgošud

Fr.: observation à haute résolution   

An observation that provides a particularly narrow, peaked image of a point source. → point spread function.

high; → resolution; → observation.

<< < -es -it -sc 201 951 abe abs abs aca acc acc aco act ada adh ado aer aft air Alf alg alk alp Alt alt amb ana And ang ani ann ant ant ant apo app app Apu arc arg Arn art ass ast ast ast atm ato att aur aut avo azi bac bal bar bar bat Bea Bel bet bia big bin bio Bir bla bla blo Blu bol Boo bou box bre Bri bro bur cal cal Can cap car Car cat cau cel cen cen cha Cha cha che Chi chr cir cir civ cla clo clo CMB coa coe 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 cri cro cry cul cur cyc D l dar dat day dea dec dec dec def def deg Del Den dep der det deu dew dic dif dif dil dip dir dis dis dis dis dis diu dog Dop dou Dra Dsc dus dwa dyn Dys Ear ecc eco edg egg Ein Ela ele ele ele ele ell eme emp enc eng ent epi equ equ equ eru eth Eur eve exa exc exe exi exo exp ext ext ext fab fai Fan fea fem fer fie fil fir fir fla fli flu foc for for for fra fre fre fri fun fuz gal gal gal Gam gau Gau gen geo geo geo geo Gib glo gov gra gra gra gra gre gro Gui H-a hal Ham har Hay hea hei hel Hel her het hie hig hoa hom hor hot Hub Hug hur hyd hyd hyl hyp ice ide ima ima imp imp inc inc ind ine inf inf inf ing inn ins ins int int int int int int int int inv inv ion iro Isl iso iso Jab jet Jov Jup Kar Kep kil Kip Kra Lag Lam Lan Lar las law lea Leg Leo lev lig lim lin lin lin lit loc loc log Lor low lum lun lun Lym Mac mag mag mag mag mag mai Mal map mas mas mat Mau mea mea med Men mer Mes Met met mic mic Mie mil min Mir mix mod mol mom Moo mor mov mul mur n-b nan nat nea neg Ner neu new New NGC noc nom non non nor nor nuc nuc nul nut obj obl obs occ oct off old one ope opp opt opt orb ord org Ori osc oth ove Owl P-s Pal par par par par Pas pat pec pen per per per per per Pha pha pho pho pho phy pie pix Pla pla pla pla Pli Poi pol pol pol pol por pos pos pow pre pre pre pre pri pri pri pro pro pro pro pro pro pro pub pul pyc qua qua qua qua qui rad rad rad rad rad rad rai 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 rur S5- Sal sat sca sca Sch sci Scu sec sec sed sel sel sem seq set sha she sho sid sie sil sim sin sit sky slo sno sod sol sol sol sol son sou spa spa spe spe spe spe sph spi spo squ sta sta sta sta ste ste ste Sti sto str str sub sub sub sul sup sup sup sup sur sur syl syn sys tal Tay tel ten ter tex the the the the Tho thr tid tim Tit too Tor tra tra Tra tra Tra tri Tri tru tub tur two Typ ult ult unc uni uni uni upl 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 > >>