Synthesis of the naturally occurring elements and their isotopes present in the Solar System solids may be divided into three broad segments: primordial nucleosynthesis (H, He), energetic particle (cosmic ray) interactions (Li, Be, B), and stellar nucleosynthesis (C and heavier elements).
In physical cosmology, Big Bang nucleosynthesis (or primordial nucleosynthesis) refers to the production of nuclei other than H-1, the normal, light hydrogen, during the early phases of the universe, shortly after the Big Bang.
Nucleosynthesis is the creation of new atomic nuclei, the centers of atoms that are made up of protons and neutrons. Nucleosynthesis first occurred within a few minutes of the Big Bang. At that time, a quark-gluon plasma, a soup of particles known as quarks and gluons, condensed into protons and neutrons.Supernova nucleosynthesis occurs in the energetic environment in supernovae, in which the elements between silicon and nickel are synthesized in quasiequilibrium established during fast fusion that attaches by reciprocating balanced nuclear reactions to 28Si.
When a star is burning hydrogen in its core, it is a main-sequence star. In older stars such as the red giants, nucleosynthesis involves the burning of heavier elements created by earlier fusion; for example, helium may burn via the triple alpha process.
Big Bang — the universe gets cool enough from quarks to form into protons and neutrons, and some of them combine by chance to form hydrogen, deuterium, helium, and lithium
Stellar — hydrogen in the core of stars fuse to form helium, and eventually heavier element up through iron
Supernova — the energy for the supernova allows for fusion of elements heavier than iron, and more importantly, spreads all the elements formed out into space instead of keeping them in a dead stellar core
The Big Bang nucleosynthesis was relatively a short in time period (first 3 minutes) due to a fast expansion of the Univers, and was able to produce only light nuclei, mainly protons and helium. Stellar nucleosynthesis started only after formation of first stars which was about few hundreds millions years later. This nucleosynthesis is a much slower process and still continues as stars live milliards of years and formation of new stars is not yet finished. Stars produce almost all nuclei up to iron , while heavier elements are produced in shorter and violent events like explosions of supernovae
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Synthesis of the naturally occurring elements and their isotopes present in the Solar System solids may be divided into three broad segments: primordial nucleosynthesis (H, He), energetic particle (cosmic ray) interactions (Li, Be, B), and stellar nucleosynthesis (C and heavier elements).
Nucleosynthesis is the creation of new atomic nuclei, the centers of atoms that are made up of protons and neutrons. Nucleosynthesis first occurred within a few minutes of the Big Bang. At that time, a quark-gluon plasma, a soup of particles known as quarks and gluons, condensed into protons and neutrons.Supernova nucleosynthesis occurs in the energetic environment in supernovae, in which the elements between silicon and nickel are synthesized in quasiequilibrium established during fast fusion that attaches by reciprocating balanced nuclear reactions to 28Si.
When a star is burning hydrogen in its core, it is a main-sequence star. In older stars such as the red giants, nucleosynthesis involves the burning of heavier elements created by earlier fusion; for example, helium may burn via the triple alpha process.
Big Bang — the universe gets cool enough from quarks to form into protons and neutrons, and some of them combine by chance to form hydrogen, deuterium, helium, and lithium
Stellar — hydrogen in the core of stars fuse to form helium, and eventually heavier element up through iron
Supernova — the energy for the supernova allows for fusion of elements heavier than iron, and more importantly, spreads all the elements formed out into space instead of keeping them in a dead stellar core
The Big Bang nucleosynthesis was relatively a short in time period (first 3 minutes) due to a fast expansion of the Univers, and was able to produce only light nuclei, mainly protons and helium. Stellar nucleosynthesis started only after formation of first stars which was about few hundreds millions years later. This nucleosynthesis is a much slower process and still continues as stars live milliards of years and formation of new stars is not yet finished. Stars produce almost all nuclei up to iron , while heavier elements are produced in shorter and violent events like explosions of supernovae