It is mostly ionized H atoms, simply protons, among free electrons (=plasma) that gets the stars going in the core. See mainly pages 3-5 of this link:Gideon said:Hi, I'm studying my astronomy course at the moment and i have question about the r- and s-process. As I understand it, in the r-process, the time between capturing two neutrons is shorter than the averge beta decay half life, right? So I'm guessing there have to be a lot of neutrons around for the r process to take place. But where do all these neutrons come from?
The r process, or rapid neutron capture process, is a nuclear reaction that occurs in supernovae explosions. It involves the rapid capture of neutrons by atomic nuclei, resulting in the creation of heavy elements. This process is responsible for the creation of about half of the elements heavier than iron in the universe.
The s process, or slow neutron capture process, is a much slower nuclear reaction that occurs in the cores of stars. It involves the capture of neutrons over a longer period of time, resulting in the creation of heavier elements. The s process is responsible for the creation of the other half of elements heavier than iron in the universe.
The r process primarily creates elements such as gold, platinum, and uranium. These elements have high atomic numbers and are considered to be some of the heaviest elements in the periodic table.
The creation of heavy elements through the r and s processes plays a crucial role in the evolution of stars and galaxies. These elements are essential for the formation of planets and the development of life. They also contribute to the energy production and dynamics of stars, and the chemical composition of galaxies.
Yes, the r and s processes can be observed in action today in various astronomical events such as supernovae explosions and neutron star mergers. These events release large amounts of energy and heavy elements into the universe, providing valuable insights into the creation of heavy elements.