AST201H1 Lecture Notes - Lecture 6: Photosphere, Blueshift, Polka

• School: UTSG
• Department: Astronomy & Astrophysics
• Course: AST201H1
• Professor: Ian Shelton

Document Summary

Why the sun remains constant and why stars do. Decline in core temp causes fusion rate to drop, so core contracts and heats up. Rise in core temp causes fusion rate to rise, so core expands and cools down. Takes thousands of years to go to the surface of the sun from the core. Through many random collisions encountered by the high energy gamma rays and particles released in the core, their energy is transferred to many other particles (atoms), each . Convection is rising hot gas = transports energy near the surface. Tell us about what sun is like inside. Data agree very well with mathematical models of the solar interior. Early searches for solar neutrinos failed to find the predicted number, measured one. More recent observations find the right number of neutrinos if we use a better type of.