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: 13176 Search : in
rural
  روستایی   
rustâyi (#)

Fr.: rural   

In, relating to, or characteristic of the → countryside.

M.E., from O.Fr. rural, from L ruralis "of the countryside," from rur-,rus "open land, country;" cf. O.E. rum "space" (extent or time); O.H.G., Gothic rum, Ger. Raum "space," ultimately from PIE root *reue- "to open; space," source also of Av. ravah- "space," O.Irish roi, roe "plain field," O.C.S. ravinu "level," Russ. ravnina "a plain."

Rustâyi, adj. of rustâ, → countryside.

Russell-Saunders coupling
  جفتش ِ راسل-ساندرز، جفسری ِ ~   
jofteš-e Russell-Saunders, jafsari-ye ~

Fr.: couplage Russell-Saunders   

A coupling scheme of → electron configuration, used mainly for the lighter atoms with → atomic number less than 30. In an atom when changes in energy states are produced by the action of two or more electrons, the value of the total angular momentum of these electrons results from the coupling between the total → orbital angular momenta of the electrons and the total → spin angular momenta of the electrons. In this scheme the orbital angular momenta and spin angular momenta of electrons are added separately to give the total angular momentum L = Σi li and the total electron spin angular momentum S = Σi si. These are then added to give J = L + S. Also called → LS coupling. See also → jj coupling.

After Henry Norris Russell (1877-1957) and Frederick Albert Saunders (1875-1963), American astronomers (1925, ApJ 61, 38); → coupling.

Russell-Vogt theorem
  فربین ِ راسل-فوکت   
farbin-e Russell-Vogt

Fr.: théorème de Russell-Vogt   

A uniqueness theorem involving the equations of state of stellar structure. → Vogt-Russell theorem.

Named after the German astronomer Heinrich Vogt (1890-1968) and the American astronomer Henry Norris Russell (1877-1957); → theorem.

rust
  زنگ   
zang (#)

Fr.: rouille   

Hydrated oxide of iron, mainly Fe2O3H2O, formed on the surface of iron when it is exposed to moisture and air.

O.E. rust, related to rudu "redness," from P.Gmc. *rusta- (cf. O.H.G., Ger. rost, M.Du. ro(e)st), from PIE base *reudh- "red" (cf. Lith. rustas "brownish," rudeti "to rust;" L. robigo, O.C.S. ruzda "rust").

Zang "rust," variants žang, zangâr, of unknown origin.

ruthenium
  روتنیوم   
ruteniom (#)

Fr.: ruthénium   

A hard, silver gray metal belonging to the → platinum group of metals; symbol: Ru. It is found directly above osmium in Group 8 of the periodic table. → Atomic number 44, → atomic weight 101.07, → melting point about 2,310°C, → boiling point about 3,900°C, → specific gravity 12.41 at 20°C.

From L. ruthenia "Russia," because it was first found by the Russian chemist Gottfried Wilhelm Osann in 1828, despite not being recognized as an element. In 1844 the Russian chemist Karl Karlovich Klaus was able to isolate the ruthenium metal.

Rutherford atom
  اتم ِ راذرفرد   
atom-e Rutherford (#)

Fr.: atome de Rutherford   

A simple model assuming that the positive charge of the atom is not distributed uniformly throughout the atom (unlike the → Thomson atom), but is concentrated in a minute center or nucleus, and the negative charge is distributed over a sphere of radius comparable with the atomic radius.

After the British physicist and chesmist Ernest Rutherford (1871-1937), who put forward this model in 1911; Nobel Prize in Chemistry in 1908; → atom.

rutherfordium
  راذرفردیوم   
râzerfordiom (#)

Fr.: rutherfordium   

An artificially produced radioactive chemical element; symbol Rf. Atomic number 104; mass number of most stable isotope 261; melting point, boiling point, and specific gravity unknown. Rutherfordium was discovered in 1964 by a team of scientists at the Joint Institute for Nuclear Research at Dubna in Russia who named the element kurchatovium. The Russian scientists were unable to duplicate their results and therefore lost credit to a team of scientists at the University of California, Berkeley, who identified the element. The scientists in California were successful in isolating the element after irradiating 249Cf with 12C.

Named after the British physicist and chemist Ernest Rutherford (1871-1937), → Rutherford atom.

rydberg
  رودبَری   
rydberg (#)

Fr.: rydberg   

A unit of energy used in atomic physics, equal to about 13.6 electron-volts, the ionization potential of hydrogen.

In honor of the Swedish physicist Johannes Robert Rydberg (1854-1919), who did important contributions on spectroscopy, and in particular found a relatively simple expression relating the various lines in the spectra of chemical elements (1890).

Rydberg constant
  پایای ِ رودبَری   
pâyâ-ye Rydberg (#)

Fr.: constante de Rydberg   

A fundamental constant of atomic physics appearing in the → Rydberg formula. The Rydberg constant for hydrogen is 109,739 cm-1.

rydberg; → constant.

Rydberg correction
  ارشایش ِ رودبَری   
aršâyeš-e Rydberg

Fr.: correction de Rydberg   

A term inserted into a formula for the energy of a single electron in the outermost shell of an atom to take into account the failure of the inner electron shells to screen the nuclear charge completely.

rydberg; → correction.

Rydberg formula
  هموگش ِ رودبَری   
hamugeš-e Rydberg

Fr.: formule de Rydberg   

A formula, used in atomic physics, which describes the wavelengths or frequencies of light in various series of related spectral lines, such as those emitted by hydrogen atoms.

rydberg; → formula.

S Andromedae
   S آندرومدا   
S Andromedâ

Fr.: S Andromedae   

The only supernova seen to date in the Andromeda galaxy and the first supernova observed beyond our own Galaxy. It was recorded on Aug. 20, 1885, by Ernst Hartwig (1851-1923) at Dorpat Observatory (Tartu) in Estonia and independently by other astronomers. S Andromedae reached magnitude 6 between Aug. 17 and 20, and had faded to magnitude 16 by February 1890. It is now believed that S Andromedae was a Type Ia supernova. Also known as SN 1885A.

S, from the second variable star to be discovered in constellation → Andromeda

S asteroid
  سیارک ِ S   
sayyârak-e S

Fr.: astéroïde S   

A moderately bright type of asteroids (albedo 0.10 to 0.22) consisting mainly of iron- and magnesium-silicates such as olivine and pyroxene. They are dominant in the inner main belt within 2.2 AU, common in the central belt within about 3 AU, but become rare further out. The largest is 15 Eunomia (about 330 km in its largest dimension).

S stands for silicaceous, → silicate; → asteroid.

S cluster
  خوشه‌ی ِ S   
xuše-ye S

Fr.: amas S   

A → star cluster situated within an arcsecond, or 0.04 pc, from the → Galactic Center, in the vicinity of the → supermassive black hole Sgr A*. The cluster members are about 40 → main sequence → B-type stars with relatively high orbital → eccentricities (0.3 ≤ e&le 0.95). The most famous member of the S cluster is S2 because of its brightness and its fast orbital motion near Sgr A*. Same as Same as the Sgr A* cluster and S stars. See also other → Galactic center clusters (Figer et al. 2002, ApJ 581, 258; and 1999, ApJ 525, 750).

S, because of proximity to → Sgr A*; → cluster.

S Doradus star
  ستاره‌ی S ِ زرین ماهی   
setâre-ye S Zarrin-mâhi

Fr.: étoiles S Doradus   

A type of massive, → blue supergiant, → variable star, also known as a → Hubble-Sandage variable or a → Luminous Blue Variable (LBV). S Doradus stars are the most luminous stars in the Galaxy and are easily identified in other nearby galaxies. They are named after the prototype, S Doradus, in the → Large Magellanic Cloud.

Dorado; → star.

S star
  ستاره‌ی ِ S   
setâre-ye S

Fr.: étoile de type S   

A → red giant of → spectral type S whose spectrum is dominated by → molecular bands arising from → zirconium → oxide (ZrO). S stars also have strong → cyanogen bands and contain spectral lines of → lithium and → technetium. Almost all S stars are → long-period variables.

S, letter of alphabet; → star.

s-process
  فراروند ِ s   
farâravand-e s

Fr.: processus s   

A → nucleosynthesis process by which → chemical elements heavier than → copper are formed through a slow flux of → neutrons absorbed by atomic nuclei (→ neutron-capture element). The → capture of neutrons occurs on time scales that are long enough to enable unstable nuclei to decay via the emission of a → beta particle before absorbing another neutron. Prominent s-process elements include → barium, → zirconium, and → yttrium. See also: → r-process.

s stands for → slow; → process.

S-type asteroid
  سیارک ِ گونه‌ی ِ S   
sayârak-e gune-ye S

Fr.: astéroïde de type S   

A type of → asteroid containing → pyroxene and → olivine silicates, probably mixed with metallic iron, similar to → stony meteorites. S-type asteroids show high albedo of 0.10-0.22. They include about 17% of known asteroids and occupy the inner → asteroid belt.

S for → stone; → type; → asteroid.

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

Fr.: étoile de type S   

Same as → S star.

S, letter of alphabet; → type; → star.

S-wave
  موج ِ S   
mowj-e S

Fr.: onde S   

shear wave.

S, referring to → shear; → wave.

<< < -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 > >>