However, only minutes are available for the 56Ni to decay within the core of a massive star. That paper defined new processes for the transformation of one heavy nucleus into others within stars, processes that could be documented by astronomers.
Image: At the end of their lives, stars with ten times the mass of our sun explode as so-called supernovae.
In interest of economy the photodisintegration rearrangement and the nuclear quasiequilibrium that it achieves is referred to as silicon burning. For about 50 years, the dominant assumption among the scientific community was that the r process took place during the final explosion of massive stars specialists speak of a core collapse supernova.
Outside the core there would be a much larger envelope consisting mainly of hydrogen and helium.
The subsequent radioactive decay of the nickel to iron keeps Type Ia optically very bright for weeks and creates more than half of all the iron in the universe. This limits their modest yields returned to interstellar gas to carbon and nitrogen, and to isotopes heavier than iron by slow capture of neutrons the s-process.