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In nuclear physics, the Bateman equation is a mathematical model describing abundances and activities in a decay chain as a function of time, based on the decay rates and initial abundances. The model was formulated by Ernest Rutherford in 1905 [1] and the analytical solution was provided by Harry Bateman in 1910. [2]
Number of isomers including stereoisomers [3] [5] Molecular Formula Name of straight chain Synonyms 1 1 1 CH 4: methane: methyl hydride; natural gas 2 1 1 C 2 H 6: ethane: dimethyl; ethyl hydride; methyl methane 3 1 1 C 3 H 8: propane: dimethyl methane; propyl hydride 4 2 2 C 4 H 10: n-butane: butyl hydride; methylethyl methane 5 3 3 C 5 H 12 ...
chain branching (a propagation step where one active particle enters the step and two or more are formed); chain transfer (a propagation step in which the active particle is a growing polymer chain which reacts to form an inactive polymer whose growth is terminated and an active small particle (such as a radical), which may then react to form a ...
The proton–proton chain, also commonly referred to as the p–p chain, is one of two known sets of nuclear fusion reactions by which stars convert hydrogen to helium. It dominates in stars with masses less than or equal to that of the Sun , [ 2 ] whereas the CNO cycle , the other known reaction, is suggested by theoretical models to dominate ...
Nuclear fusion reaction of two helium-4 nuclei produces beryllium-8, which is highly unstable, and decays back into smaller nuclei with a half-life of 8.19 × 10 −17 s, unless within that time a third alpha particle fuses with the beryllium-8 nucleus [3] to produce an excited resonance state of carbon-12, [4] called the Hoyle state, which ...
In organic chemistry, pentadiene is any hydrocarbon with an open chain of five carbons, connected by two single bonds and two double bonds. All those compounds have the same molecular formula C 5 H 8. The inventory of pentadienes include: 1,2-pentadiene, or ethyl allene, H 2 C=C=CH−CH 2 −CH 3. [1] 1,3-pentadiene, H 2 C=CH−CH=CH−CH 3 ...
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In stars between 4 and 11 solar masses, the 16 O already produced by helium fusion in the previous stage of stellar evolution manages to survive the carbon-burning process pretty well, despite some of it being used up by capturing 4 He nuclei. [1] [8] So the result of carbon burning is a mixture mainly of oxygen, neon, sodium and magnesium. [3] [5]