Lecture 14: Star Formation
Update: 2006-01-24
Description
How do stars form? The Sun is old and in Hydrostatic and
Thermal equilibrium. How did it get that way? This lecture
presents the basic steps of star formation as a progress from
cold interstellar Giant Molecular Clouds to Protostars in
Hydrostatic Equilibrium, and then Pre-Main Sequence evolution
which ends in ignition of core Hydrogen fusion and establishing
Thermal Equilibrium on the Zero-Age Main Sequence.
Recorded 2006 January 24 in 1008 Evans Laboratory on the Columbus campus
of The Ohio State University.
Thermal equilibrium. How did it get that way? This lecture
presents the basic steps of star formation as a progress from
cold interstellar Giant Molecular Clouds to Protostars in
Hydrostatic Equilibrium, and then Pre-Main Sequence evolution
which ends in ignition of core Hydrogen fusion and establishing
Thermal Equilibrium on the Zero-Age Main Sequence.
Recorded 2006 January 24 in 1008 Evans Laboratory on the Columbus campus
of The Ohio State University.
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