ASTR 114 Lecture Notes - Lecture 16: Convection Zone, Radiation Zone, Photosphere
10 Jan 2020
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Document Summary
Layers compress lower layers -5. 67 x 10^-8 w/m^2k^4. Physical properties of the sun: the core is where nuclear fusion occurs. Luminosity: total energy radiated by the sun (can be calculated from amount reaching earth) Solar constant: amount of sun"s energy reaching earth- the sun is stable b/c the weight of upper. Gravitational equilibrium: an inward gravitational must be balanced by outward pressure. Energy balance: the rate at which energy radiated from the surface of the sun must be the same as the. Fission: big nucleus splits into smaller pieces (nuclear power plants) Fusion: small nucleus sticks together to make a bigger one (the sun, stars) (high temperatures) Proton-proton chain: how hydrogen fuses into helium in sun. Core: sun releases energy by fusing 4 hydrogen nucleus and helium nucleus. Neutrinos: neutrinos created during fusion fly directly through the sun (observations tell us what is happening in the core) (rarely interact with matter)
