Stellar evolution traces the life of a star from its birth in a collapsing molecular cloud through hydrogen fusion on the main sequence, to its final fate as a white dwarf, neutron star, or black hole. The mass of a star at birth determines its luminosity, temperature, lifetime, and ultimate demise — a relationship beautifully captured by the Hertzsprung-Russell diagram.
These simulations let you plot stars on the HR diagram, model main-sequence energy output, watch white dwarfs cool over billions of years, trace nucleosynthesis element production, and explore the Chandrasekhar limit that separates white dwarfs from catastrophic collapse — all with real-time interactive controls and physically accurate stellar models.