Lecture 11: The Internal Structure of Stars
What are the physical laws that determine the internal structure\nof stars? We first introduce the Mass-Luminosity Relation for\nMain Sequence stars, as well as seeing how the mean density of stars\ndiffers for stars on different parts of the H-R diagram. We then\nintroduce the Ideal Gas Law, which relates pressure, density, and temperature,\nand show how the internal structure of a star is determined by\na continuous tug-of-war between internal pressure trying to blow\nthe star apart, and self-gravity trying to make it collapse. The\nbalance between the two is the state of Hydrostatic Equilibrium. How\nthe balance is maintained, and what happens when it is tipped in\nfavor of either will determine the appearance and subsequent evolution\nof the star. Recorded 2006 January 18 in 1008 Evans Laboratory on the \nColumbus campus of The Ohio State University.