sruthisupriya
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could anyone explain p-process in nucleosynthesis for me? i didnt find any suitable site.
The p-process in nucleosynthesis refers to a type of nuclear reaction occurring during the early stages of a supernova explosion, resulting in the formation of neutron-deficient isotopes of elements ranging from krypton to zirconium. This process involves the capture of protons by nuclei formed through the r-process and s-process. Key resources for understanding the p-process include the paper "The p-process in supernovae" by Woosley and Howard, as well as various online lectures and articles that detail the conditions necessary for this synthesis, particularly at peak temperatures of 2 to 3 billion K.
PREREQUISITESAstronomers, astrophysicists, and students studying stellar nucleosynthesis and supernova phenomena will benefit from this discussion.
sruthisupriya said:could anyone explain p-process in nucleosynthesis for me? i didnt find any suitable site.
http://www.daviddarling.info/encyclopedia/P/p-process.htmlA type of nuclear reaction thought to occur in the early stages of a supernova explosion that results in the formation of certain neutron-deficient isotopes of elements from krypton to zirconium. It involves the capture of protons by nuclei previously formed by the r-process and the s-process.
The nucleosynthetic origin of the rare proton-rich isotopes, usually called 'p-process' isotopes, is examined. A particularly interesting context for this synthesis is found to be explosive events characterized by peak temperatures in the range from 2 to 3 billion K. At these temperatures a series of photodisintegration reactions operating upon a distribution of r- and s-process seeds produces an abundance pattern that displays striking similarities to that of the p-process nuclei in the solar system. The large proton densities usually required for such synthesis are not needed. Requisite conditions for this model are expected to occur naturally in those zones of supernovae that have experienced helium and perhaps carbon burning prior to explosion. Implications for supernova structure, presupernova evolution, and cosmochronology are discussed, and a critical discussion of other current p-process models is presented.