Hydrostatic equilibrium: negative feedback loop If core T drops, • fusion rate drops, • core contracts • heats up If core heats up, • fusion rate rises • core expands • cools down
Main sequence stars are modeled as concentric spherical shells in hydrostatic equilibrium Mass element dm Constant density Inward force = outward force
Binding energy holds a nucleus together: BE = total mass of each individual nucleon - mass of nucleus
The Coulomb barrier: 1 in 1085 particles has the energy to cross it
Wave function Probability distribution
Quantum tunneling
Gamow Peak: energy region where the reaction is more likely to take place Can’t tunnel through Coulomb barrier Few particles
Another view of Gamow peak
One of 3 branches of proton-proton chain
CNO cycle: C, N O atoms act as catalysts
T-dependence of pp chain and CNO cycle
Solar neutrino problem: Early searches for solar neutrinos only found ~1/3 the expected number of neutrinos
Solar neutrino problem: Early searches for solar neutrinos only found ~1/3 the expected number of neutrinos Neutrinos apparently can change form. According to nuclear physics theory, this means they must have mass! “flavor oscillation”
Super-Kamiokande in Japan. • 1 km underground (in a mine) • 11, 000 light-detectors in/around a pool of water • Neutrino can (rarely) interact with a proton • A particle is produced that moves faster than the speed of light in water • Causes an optical “sonic boom”