Stellar Nucleosynthesis: The Creation of Elements in Stars

Stellar Nucleosynthesis is the process by which elements heavier than iron are created inside stars through nuclear fusion reactions.

The Proton-Proton Chain is the primary mechanism for energy production in main-sequence stars with masses less than about 1.5 solar masses.

The triple-alpha process is a series of nuclear fusion reactions that converts three helium nuclei into a carbon nucleus.

The R-Process is a rapid neutron capture process that occurs during supernovae and produces elements heavier than iron.

The s-process is a slow neutron capture process that occurs in asymptotic giant branch stars and produces elements heavier than iron.

Big Bang Nucleosynthesis is the process that created the lightest elements (hydrogen, helium, lithium, beryllium, and boron) in the early universe.

Massive stars (with masses greater than about 8 solar masses) are most likely to undergo a supernova at the end of their lives.

Helium is the most abundant element produced during stellar nucleosynthesis.

The CNO Cycle is a series of nuclear fusion reactions that converts hydrogen into helium and produces elements such as sodium, magnesium, and aluminum.

Uranium is the most abundant element produced during the r-process.

Main-sequence stars are the most likely to produce elements such as carbon, nitrogen, and oxygen through nuclear fusion reactions.

Cosmic Ray Nucleosynthesis is the process that produces elements such as lithium, beryllium, and boron in stars through the interaction of cosmic rays with interstellar gas.

Supernovae are the most likely to produce elements such as iron and nickel through the r-process.

The CNO Cycle is the process that produces elements such as carbon, nitrogen, and oxygen in stars through nuclear fusion reactions.

Supernovae are the most likely to produce elements such as lead, uranium, and thorium through the r-process.