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.