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nuclear fusion 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 magnetic resonance (NMR) 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 ^{1}H, ^{13}C, ^{29}Si, or ^{31}P) 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 magnetism meqnâtis-e haste-yi (#) Fr.: magnétisme nucléaire The magnetism associated with the magnetic field generated by atomic nuclei. |
nuclear mass 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 physics 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 power tavân-e haste-yi Fr.: puissance nucléaire Electric or motive power whose primary source is nuclear energy. |
nuclear process 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 reaction vâžireš-e haste-yi Fr.: réaction nucléaire A process in which the energy, composition, or structure of an atomic nucleus changes. |
nuclear reactor 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 spin 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 statistical equilibrium (NSE) 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 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 m_{H}. Therefore, the maximum amount of energy a star with a hydrogen mass M can release is Δ M = 0.008 Mc^{2}. The nuclear time scale is then: t = 0.008 c^{2}M/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 10^{10} years. |
nuclear transition 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 tarâmuteš-e haste-yi Fr.: transmutation nucléaire The changing of atoms of one element into those of another by suitable nuclear reactions. → nuclear; → transmutation. |
nuclear waste âxâl-e haste-yi (#) Fr.: déchets nucléaires A particular type of radioactive waste that is produced as part of the nuclear fuel cycle. These include extraction of uranium from ore, concentration of uranium, processing into nuclear fuel, and disposal of byproducts. |
nucleon haston Fr.: nucléon A constituent of the atomic nucleus, i.e. a proton or a neutron. From nucle(us), → nucleus, + -on a suffix used in the names of subatomic particles, probably extracted from → ion. Haston, from hast(é)→ nucleus + -on, as above. |
nucleonics hastonik Fr.: nucléonique The practical applications of nuclear physics, and the techniques associated with those applications. |
nucleosynthesis haste-handâyeš Fr.: nucléosynthèse The process by which → nuclear reactions at very high temperatures and pressures produce the various → chemical elements of the → periodic table, either in the → Big Bang or in stellar interiors. See also → primordial nucleosynthesis, → stellar nucleosynthesis, → explosive nucleosynthesis. |
nucleosynthesize haste-handâyidan Fr.: nucléosynthétiser Produce through → nucleosynthesis. → nucleosynthesis; → -ize. |
nucleosynthetic haste-handâyeši Fr.: nucléosynthétique Of, pertaining to, proceeding by, or involving → nucleosynthesis. Adj. of → nucleosynthesis. |
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