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The materials that made up the solar system can be studied through the analysis of pre-solar grains and the abundances of various isotopes in primitive meteoritic material. Pre-solar grains were formed in the photospheres of stars pre-dating the Sun. These grains were then expelled into the interstellar medium (ISM) in stellar winds and also in supernova ...


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The "weight" must surely refer to the atomic weight which is just the sum of the number of protons and neutrons. i.e. for Iron it is (usually) 56. Many of the chemical elements heavier than iron are formed inside giant stars via the s-process. This is the slow neutron capture onto iron-peak seed nuclei. It is normally termed "neutron capture", but I suppose ...


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Practically all the elements heavier than lead are created by neutron capture in the r-process. This requires the explosive conditions of a supernova or neutron star merger. In terms of some limit, I'm not sure how to answer. Stuff that's heavier than Uranium has a short half life compared to the age of the Earth, so there's not much to be found. They may ...



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