zanjir (#), zanjiré (#)
Chain, from O.Fr. chaeine, from L. catena "fetter."
Zanjir from Mid.Pers. zanjir "chain;" zanjiré, from zanjir + nuance suffix -é.
vâžireš-e zanjiri, vâkoneš-e ~
Fr.: réaction en chaîne
A succession of → nuclear fissions when the neutrons released by previous fissions produce other nuclear fissions which themselves cause other reactions and the reactions goes on increasing exponentially.
Fr.: chaîne de désintégration
A series of nuclear decays produced by successive → daughter products, when the daughters are themselves → radioactive. For example, the decay chain N1→ N2→ N3→ ... in which the parent nuclide N1 decays to the daughter N2, which in turn decays to N3. Each → radionuclide in the decay chain can → branch to more than one daughter.
Fr.: chaîne de Markarian
A string of a dozen or so galaxies in the central region of the → Vigo cluster. The chain lies to the right of the cluster's dominant galaxy M87 and extends over nearly 2° on the sky. The chain's brightest galaxies are the lenticulars M84 and M86. At least seven galaxies in the chain appear to move coherently, although others appear to be superposed by chance.
zanjire-ye Markov (#)
Fr.: chaîne de Markov
A → stochastic process, based on the classical → random walk concept, in which the probabilities of occurrence of various future states depend only on the previous state of the system and not on any of earlier states. Also called Markov process and Markovian principle.
Named after Andrey Andreyevich Markov (1856-1922), a Russian mathematician, who introduced this model in 1906; → chain.
Markov Chain Monte Carlo (MCMC)
raveš-e Monte Carlo bâ zanjire-ye Markov
Fr.: Méthode de Monte-Carlo par chaînes de Markov
A method for sampling from → probability distributions using → Markov chains. MCMC methods are widely used in data modeling for → Bayesian inference and numerical integration in physics, chemistry, biology, statistics, and computer science.
zanjire-ye proton-proton (#)
Fr.: chaîne proton-proton
A series of → thermonuclear reactions, taking place mainly in → low-mass stars, such as the Sun, which transforms four hydrogen nuclei (protons) into one helium (4He) nucleus and thereby generates energy in the stellar core. First, two protons (1H) combine to form a → deuterium nucleus (2H) with the emission of a → positron (e+) and a → neutrino (ν): 1H + 1H → 2H + e+ + ν. The deuterium nucleus then rapidly captures another proton to form a helium-3 nucleus (3He), while emitting a → gamma ray (γ): 2H + 1H → 3He + γ. There are three alternatives for the next step. In the PP I chain, occurring in 86% of the cases, two 3He nuclei fuse to a final 4He nucleus while two protons are released: 3He + 3He → 4He + 1H + 1H. The mass of the resulting 4He nucleus is less than the total mass of the four original protons used to produce 4He (→ mass defect). The difference, ~ 0.7% of the total mass of the protons, is converted into energy and radiated by the Sun. In this process, the Sun loses some 4 million tons of its mass each second. See also → CNO cycle.