01
Star Formation
Stars form from gravitationally collapsing regions of molecular clouds. As material contracts, gravitational potential energy is converted into thermal energy and the protostellar system evolves toward nuclear ignition.
02
Hydrostatic Equilibrium
A main-sequence star maintains approximate hydrostatic equilibrium: gravity pulls inward while pressure generated by the hot interior supports the star.
03
Stellar Evolution
- Main-sequence hydrogen burning.
- Post-main-sequence expansion.
- Helium burning in appropriate stellar masses.
- Advanced nuclear burning in massive stars.
- Final compact remnants.
04
Stellar Remnants
- White dwarfs.
- Neutron stars.
- Black holes.