IB Physics SL E.5.4 Stellar mass & evolution
IB Physics SL E.5.4 Stellar mass & evolution
Practise using luminosity equations and stellar-mass evidence to predict main-sequence lifetime, fusion rate and final stellar remnant.
How this is tested
- use the equation L proportional to M^3.5 to calculate stellar mass before predicting the final remnant
- combine L = E/t with E proportional to M to compare main-sequence lifetimes from mass
- use the mass decision, not HR-diagram position alone, to choose white dwarf, neutron star or black hole