STAR LIFE CYCLE & EVOLUTION SIMULATOR
In the cosmos, mass is destiny. Adjust the starting mass of a newborn star to discover its fusion power, lifetime, and ultimate celestial fate.
1.00 M☉ (Solar Masses)
0.1 M☉ (Red Dwarf)
1.0 M☉ (Sun)
8.0 M☉ (Supernova Threshold)
25 M☉ (Black Hole Threshold)
60 M☉ (Hypergiant)
Class: G-Type Yellow Dwarf
Final Fate: White Dwarf
10.0 Billion Yrs
Main Sequence Lifespan
1.00 L☉
Relative Luminosity ($L \propto M^{3.5}$)
5,778 K
Surface Temperature
Evolutionary Life Path
Nuclear Fusion Mechanics
Why Bigger Stars Live Shorter Lives
You might assume that having 20 times more hydrogen fuel would let a massive star burn 20 times longer. The opposite is true!
Because gravitational pressure increases exponentially with mass, the core temperature skyrockets, accelerating fusion at an astronomical rate ($L \propto M^{3.5}$). A 20-solar-mass blue giant burns through its immense fuel reserves in barely 10 million years, whereas a thrifty 0.2-solar-mass red dwarf will steadily sip its fuel for several trillion years—far longer than the current age of our universe (13.8 billion years)!