Lecture 15: The Main Sequence
Update: 2006-01-25
Description
What are the properties of stars on the Main Sequence? This lecture
discusses what happens to a star after it alights onto the Main
Sequence, burning H to He in its core, and maintaining a state
of Hydrostatic and Thermal Equilibrium. We will see how the mass
of a star determines its location along the Main Sequence and
influences its energy generation and internal structure. We finally
introduce the nuclear timescale and derive the Main-Sequence Lifetime
for stars, and discuss its consequences.
Recorded 2006 January 25 in 1008 Evans Laboratory on the Columbus campus
of The Ohio State University.
discusses what happens to a star after it alights onto the Main
Sequence, burning H to He in its core, and maintaining a state
of Hydrostatic and Thermal Equilibrium. We will see how the mass
of a star determines its location along the Main Sequence and
influences its energy generation and internal structure. We finally
introduce the nuclear timescale and derive the Main-Sequence Lifetime
for stars, and discuss its consequences.
Recorded 2006 January 25 in 1008 Evans Laboratory on the Columbus campus
of The Ohio State University.
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