enow.com Web Search

Search results

  1. Results from the WOW.Com Content Network
  2. Nuclear fusion - Wikipedia

    en.wikipedia.org/wiki/Nuclear_fusion

    Nuclear fusion uses lighter elements, such as hydrogen and helium, which are in general more fusible; while the heavier elements, such as uranium, thorium and plutonium, are more fissionable. The extreme astrophysical event of a supernova can produce enough energy to fuse nuclei into elements heavier than iron.

  3. Synthesis of precious metals - Wikipedia

    en.wikipedia.org/wiki/Synthesis_of_precious_metals

    The longest half-lives of the radioisotopes of these elements generated by nuclear fission are 373.59 days for ruthenium and 45 days for rhodium [clarification needed]. This makes the extraction of the non-radioactive isotope from spent nuclear fuel possible after a few years of storage, although the extract must be checked for radioactivity ...

  4. Alpha process - Wikipedia

    en.wikipedia.org/wiki/Alpha_process

    The stable alpha elements are: C, O, Ne, Mg, Si, and S. The elements Ar and Ca are "observationally stable". They are synthesized by alpha capture prior to the silicon fusing stage, that leads to Type II supernovae. Si and Ca are purely alpha process elements. Mg can be separately consumed by proton capture reactions.

  5. Triple-alpha process - Wikipedia

    en.wikipedia.org/wiki/Triple-alpha_process

    Based on known resonances, by 1952 it seemed impossible for ordinary stars to produce carbon as well as any heavier element. [14] Nuclear physicist William Alfred Fowler had noted the beryllium-8 resonance, and Edwin Salpeter had calculated the reaction rate for 8 Be, 12 C, and 16 O nucleosynthesis taking this resonance into account.

  6. r-process - Wikipedia

    en.wikipedia.org/wiki/R-process

    Abundance peaks for the r-process occur near mass numbers A = 82 (elements Se, Br, and Kr), A = 130 (elements Te, I, and Xe) and A = 196 (elements Os, Ir, and Pt). The r-process entails a succession of rapid neutron captures (hence the name) by one or more heavy seed nuclei, typically beginning with nuclei in the abundance peak centered on 56 Fe.

  7. Stellar nucleosynthesis - Wikipedia

    en.wikipedia.org/wiki/Stellar_nucleosynthesis

    The need for a physical description was already inspired by the relative abundances of the chemical elements in the solar system. Those abundances, when plotted on a graph as a function of the atomic number of the element, have a jagged sawtooth shape that varies by factors of tens of millions (see history of nucleosynthesis theory). [4]

  8. AOL Mail

    mail.aol.com

    Get AOL Mail for FREE! Manage your email like never before with travel, photo & document views. Personalize your inbox with themes & tabs. You've Got Mail!

  9. Alpha particle - Wikipedia

    en.wikipedia.org/wiki/Alpha_particle

    After five years of additional experimental work, Rutherford and Hans Geiger determined that "the alpha particle, after it has lost its positive charge, is a Helium atom". [7] [8] [9]: 61 Alpha radiation consists of particles equivalent to doubly-ionized helium nuclei (He 2+) which can gain electrons from passing through matter. This mechanism ...