Supernovae and nucleosynthesis
Nucleogenesis of the elements
Entirely new astronomical data about the r-process was discovered in when the LIGO and Virgo gravitational-wave observatories discovered a merger of two neutron stars that had previously been orbiting one another  That can happen when both massive stars in orbit with one another become core-collapse supernovae, leaving neutron-star remnants. In the r-process, any heavy nuclei are bombarded with a large neutron flux to form highly unstable neutron rich nuclei which very rapidly undergo beta decay to form more stable nuclei with higher atomic number and the same atomic mass. Sparvoli, P. Gerhardt, A. Download preview PDF. Yurkin, G. Paul, R. Goodman, Z.
Hoyle, Gamma-ray lines from novae. The explosive burning caused when the supernova shock passes through the silicon-burning shell lasts only seconds but is the major contributor to nucleosynthesis in the mass range Tibolla, K.
Bellazzini, B. Ukwatta, G. During supernova nucleosynthesis, the r-process creates very neutron-rich heavy isotopes, which decay after the event to the first stable isotopethereby creating the neutron-rich stable isotopes of all heavy elements. Tollefson, I.
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