Lecture 15: The Main Sequence
What are the properties of stars on the Main Sequence? This lecture\ndiscusses what happens to a star after it alights onto the Main\nSequence, burning H to He in its core, and maintaining a state\nof Hydrostatic and Thermal Equilibrium. We will see how the mass\nof a star determines its location along the Main Sequence and\ninfluences its energy generation and internal structure. We finally\nintroduce the nuclear timescale and derive the Main-Sequence Lifetime\nfor stars, and discuss its consequences.\nRecorded 2006 January 25 in 1008 Evans Laboratory on the Columbus campus\nof The Ohio State University.