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  2. Nucleosynthesis - Wikipedia

    en.wikipedia.org/wiki/Nucleosynthesis

    The first direct proof that nucleosynthesis occurs in stars was the astronomical observation that interstellar gas has become enriched with heavy elements as time passed. As a result, stars that were born from it late in the galaxy, formed with much higher initial heavy element abundances than those that had formed earlier.

  3. 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]

  4. 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.

  5. Supernova nucleosynthesis - Wikipedia

    en.wikipedia.org/wiki/Supernova_nucleosynthesis

    Supernova nucleosynthesis is the nucleosynthesis of chemical elements in supernova explosions.. In sufficiently massive stars, the nucleosynthesis by fusion of lighter elements into heavier ones occurs during sequential hydrostatic burning processes called helium burning, carbon burning, oxygen burning, and silicon burning, in which the byproducts of one nuclear fuel become, after ...

  6. Neutron capture - Wikipedia

    en.wikipedia.org/wiki/Neutron_capture

    Neutron capture plays a significant role in the cosmic nucleosynthesis of heavy elements. In stars it can proceed in two ways: as a rapid process ( r-process ) or a slow process ( s-process ). [ 1 ] Nuclei of masses greater than 56 cannot be formed by exothermic thermonuclear reactions (i.e., by nuclear fusion ) but can be formed by neutron ...

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  8. Big Bang nucleosynthesis - Wikipedia

    en.wikipedia.org/wiki/Big_Bang_nucleosynthesis

    Although the baryon per photon ratio is important in determining element abundances, the precise value makes little difference to the overall picture. Without major changes to the Big Bang theory itself, BBN will result in mass abundances of about 75% of hydrogen-1, about 25% helium-4 , about 0.01% of deuterium and helium-3 , trace amounts (on ...

  9. B2FH paper - Wikipedia

    en.wikipedia.org/wiki/B2FH_paper

    The B 2 FH paper argued that when a star dies, it will enrich the interstellar medium with 'heavy elements' (in this case all elements heavier than lithium), from which newer stars are formed. The B 2 FH paper described key aspects of the nuclear physics and astrophysics involved in how stars produce these heavy elements.