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Neutron flux in asymptotic giant branch stars and in supernovae is responsible for most of the natural nucleosynthesis producing elements heavier than iron.In stars there is a relatively low neutron flux on the order of 10 5 to 10 11 cm −2 s −1, resulting in nucleosynthesis by the s-process (slow neutron-capture process).
Artist's conception of a powerful magnetar in a star cluster. A magnetar is a type of neutron star with an extremely powerful magnetic field (~10 9 to 10 11 T, ~10 13 to 10 15 G). [1] ...
The s-process is believed to occur mostly in asymptotic giant branch stars, seeded by iron nuclei left by a supernova during a previous generation of stars. In contrast to the r-process which is believed to occur over time scales of seconds in explosive environments, the s-process is believed to occur over time scales of thousands of years, passing decades between neutron captures.
One hypothesis is that of "flux freezing", or conservation of the original magnetic flux during the formation of the neutron star. [40] If an object has a certain magnetic flux over its surface area, and that area shrinks to a smaller area, but the magnetic flux is conserved, then the magnetic field would correspondingly increase. Likewise, a ...
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 ...
Neutron stars are the collapsed cores of supergiant stars. [1] They are created as a result of supernovas and gravitational collapse, [2] and are the second-smallest and densest class of stellar objects. [3] In the cores of these stars, protons and electrons combine to form neutrons. [2] Neutron stars can be classified as pulsars if they are ...
A massive star collapses at the end of its life, emitting on the order of 10 58 neutrinos and antineutrinos in all lepton flavors. [2] The luminosity of different neutrino and antineutrino species are roughly the same. [3] They carry away about 99% of the gravitational energy of the dying star as a burst lasting tens of seconds.
R-process describes neutron capture in a region of high neutron flux, such as during supernova nucleosynthesis after core-collapse, and yields neutron-rich nuclides. S-process describes neutron capture that is slow relative to the rate of beta decay, as for stellar nucleosynthesis in some stars, and yields nuclei with stable nuclear shells.