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
nuclear cross-section
  سکنج‌گاه ِ هسته‌ای   
sekanjgâh-e hasteyi

Fr.: section efficace nucléaire   

Apparent cross-section possessed by an atomic nucleus when it undergoes a particular type of collision process.

nuclear; → cross section.

nuclear density
  چگالی ِ هسته‌ای   
cagâli-ye haste-yi (#)

Fr.: densité nucléaire   

The density of an atomic nucleus (about 1014 g/cm3).

nuclear; → density.

nuclear energy
  کاروژ ِ هسته‌ای   
kâruž-e haste-yi

Fr.: énergie nucléaire   

Energy released during a nuclear reaction as the result of the conversion of mass into energy. → mass-energy equivalence.

nuclear; → energy.

nuclear fission
  شکافت ِ هسته‌ای   
šekâft-e haste-yi (#)

Fr.: fission nucléaire   

A → nuclear reaction in which a heavy atomic nucleus splits into two or more approximately equal parts, usually as the result of the capture of a slow, or → thermal neutron by the nucleus. It is normally accompanied by the emission of further neutrons or → gamma rays and very large amounts of energy. The neutrons can continue the process as a → chain reaction, so that it becomes the source of energy in a → nuclear reactor or an atomic bomb. It may also be a trigger for → nuclear fusion in a hydrogen bomb. Fission occurs spontaneously in nuclei of uranium-235, the main fuel used in nuclear reactors.

nuclear; → fission.

nuclear force
  نیروی ِ هسته‌ای   
niru-ye haste-yi (#)

Fr.: force nucléaire   

The attractive force which acts between nucleons when they are extremely close together (closer than 10-13 cm).

nuclear; → force.

nuclear fuel
  سوخت ِ هسته‌ای   
suxt-e haste-yi (#)

Fr.: combustible nucléaire   

A substance, such as uranium-238 or plutonium-239, which undergoes nuclear fission in a nuclear reactor.

nuclear; → fuel.

nuclear fusion
  ایوش ِ هسته‌ای   
iveš-e haste-yi

Fr.: fusion nucléaire   

A → nuclear reaction between atomic nuclei as a result of which a heavier → atomic nucleus is formed, a small fraction of mass is lost, and a large quantity of energy is released. Nuclear fusion is the source of the energy of stars.

nuclear; → fusion.

nuclear magnetic resonance (NMR)
  باز‌آوایی ِ مغناتیسی ِ هسته‌ای   
bâzâvâyi-ye meqnâtisi-ye haste-yi

Fr.: résonance magnétique nucléaire   

An analysis technique applied to some atomic nuclei that have the property to behave as small magnets and respond to the application of a magnetic field by absorbing or emitting electromagnetic radiation. When nuclei which have a magnetic moment (such as 1H, 13C, 29Si, or 31P) are submitted to a constant magnetic field and at the same time to a radio-frequency alternating magnetic field, the nuclear magnetic moment is excited to higher energy states if the alternating field has the specific resonance frequency. This technique is especially used in spectroscopic studies of molecular structure and in particular provides valuable information in medicine that can be used to deduce the structure of organic compounds.

nuclear; → magnetic; → resonance.

nuclear magnetism
  مغناتیس ِ هسته‌ای   
meqnâtis-e haste-yi (#)

Fr.: magnétisme nucléaire   

The magnetism associated with the magnetic field generated by atomic nuclei.

nuclear; → magnetism.

nuclear mass
  جرم ِ هسته‌ای   
jerm-e haste-yi (#)

Fr.: masse nucléaire   

The quantity of matter in a nucleus, which is less than the total mass of its nucleons by its binding energy divided by the square of the speed of light.

nuclear; → mass.

nuclear physics
  فیزیک ِ هسته‌ای   
fizik-e haste-yi

Fr.: physique nucléaire   

The branch of physics which is concerned with the study of atomic nuclei, subatomic particles, and their exploitation.

nuclear; → physics.

nuclear power
  توان ِ هسته‌ای   
tavân-e haste-yi

Fr.: puissance nucléaire   

Electric or motive power whose primary source is nuclear energy.

nuclear; → power.

nuclear process
  فراروند ِ هسته‌ای   
farâravand-e haste-yi

Fr.: processus nucléaire   

A process in which an → atomic nucleus changes, including → radioactive decay of naturally occurring and man-made → isotopes, → nuclear fission, and → nuclear fusion.

nuclear; → process.

nuclear reaction
  واژیرش ِ هسته‌ای   
vâžireš-e haste-yi

Fr.: réaction nucléaire   

A process in which the energy, composition, or structure of an atomic nucleus changes.

nuclear; → reaction.

nuclear reactor
  واژیرگر ِ هسته‌ای   
vâžirgar-e haste-yi

Fr.: réacteur nucléaire   

A device in which a nuclear fission chain reaction is maintained and controlled for the production of nuclear energy or radioactive isotopes.

nuclear; → reactor.

nuclear spin
  اسپین ِ هسته‌ای   
espin-e haste-yi

Fr.: spin nucléaire   

The total → angular momentum of a → nucleus, represented by symbol I. The nucleus, which is composed of neutrons and protons, acts as if it is a single entity which has intrinsic angular momentum. The nuclear spin depends on the → mass number; if the mass number is odd then the nucleus has half-integer spin like the electron while if the nucleus has even mass number then its spin will be integer spin.

nuclear; → spin.

nuclear statistical equilibrium (NSE)
  ترازمندی ِ آماری ِ هسته‌ای   
tarâzmandi-ye âmâri-ye haste-yi

Fr.: équilibre statistique nucléaire   

In → nucleosynthesis models, the condition in which all nuclear species are in equilibrium under exchange of → protons and → neutrons. Matter in nuclear statistical equilibrium is characterized by a large abundance of iron peak nuclei. In such equilibria abundance of each nuclide can be calculated from repeated application of → Saha equation.

nuclear; → statistical; → equilibrium.

nuclear time scale
  مرپل ِ زمانی ِ هسته‌ای   
marpel-e zamâni-ye haste-yi

Fr.: échelle de temps nucléaire   

The time required for a star to exhaust its hydrogen (H) supply in → nuclear fusion. The nuclear time scale is given by the relation t = E/L, where E is the total nuclear energy that can be generated by a star and L is the stellar → luminosity. Assuming that the end point of fusion is → iron (Fe), the → atomic mass difference between H and Fe is Δm = 0.008 mH. Therefore, the maximum amount of energy a star with a hydrogen mass M can release is Δ M = 0.008 Mc2. The nuclear time scale is then: t = 0.008 c2M/L. However, stars use up only a fraction of their hydrogen supply, because only the inner part of the star is hot enough for fusion. For example, the Sun will spend only about 10% of its hydrogen supply before evolving into a → red giant. In other words, the solar life time on the → main sequence is about 1010 years.

nuclear; → time; → scale.

nuclear transition
  گذرش ِ هسته‌ای   
gozareš-e haste-yi

Fr.: transition   

A change in the → energy level or state of an atomic → nucleus involving a → quantum of energy.

nuclear; → transition.

nuclear transmutation
  تراموتش ِ هسته‌ای   
tarâmuteš-e haste-yi

Fr.: transmutation nucléaire   

The changing of atoms of one element into those of another by suitable nuclear reactions.

nuclear; → transmutation.

<< < -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 > >>