Stellar Evolution 3D Interactive Simulation

What you'll learn

• How a star's initial mass permanently dictates its evolutionary sequence.
• The physical transformations during the Main Sequence, Red Giant, and final remnant stages.
• The relationship between core temperature, physical radius, and luminosity.

How to use it

1. Select an initial stellar mass (0.05 to 150 Solar Masses) using the control panel.
2. Drag the timeline scrubber to advance time and observe structural changes in real-time.
3. Monitor the telemetry panel to track live temperature, radius, and luminosity values.

Notes

This robust simulation uses proportional visualisations and real-time telemetry to clearly demonstrate complex astrophysical concepts. It is an excellent visual aid for GCSE and A-Level astrophysics modules.