Stellar Nucleosynthesis Explorer
Investigate how stars produce elements over their life cycles. Select an initial mass, advance through the stages, and observe the fusion processes.
Simulation Controls
1.0 Solar Masses
Age: 0%
Stellar Diagnostics
Current Stage
Protostar
Core Temp
< 10M K
Primary Core Reaction
Gravitational Contraction
Elements Produced/Present
Nucleon Conservation Analysis
Analyze the current core reaction. During nuclear fusion, atoms change, but the total number of protons (P) and neutrons (N) is conserved.
Waiting for fusion to begin...
CCC: Energy and Matter. In nuclear processes, atoms are not conserved, but the total number of protons plus neutrons is conserved.
Evolution Data Log
| Stage | Temp (approx) | Heaviest |
|---|
Stellar Report Card
Initial Parameters
Solar Masses
Final Remnant
Nucleosynthesis Summary: Elements Produced
Nucleon Conservation Principle
Throughout the star's life cycle, lighter elements were fused into heavier elements. During every nuclear reaction, while the atoms themselves changed, the total number of protons and neutrons (nucleons) was conserved.