Calculateur de Relation Masse-Luminosité
Calculez la luminosité d'une étoile à partir de sa masse.
Luminosité (L_sun)
1.0000 L_sun
Luminosity (L_sun) vs Stellar Mass
Formule
## Mass-Luminosity Relation For main-sequence stars, luminosity increases steeply with mass: **L / L_sun ≈ (M / M_sun)^3.5** This is an empirical fit. The exponent varies from about 2.3 for very low-mass stars to about 4 for massive stars, with 3.5 being a good average. A 10 M_sun star is ~3162 times as luminous as the Sun.
Exemple Résolu
A 2 solar-mass star.
- 01L/L_sun = 2^3.5
- 02= 2^3 × 2^0.5 = 8 × 1.414 = 11.31
- 03About 11.3 times the Sun's luminosity.
Questions Fréquentes
Why does luminosity rise so steeply with mass?
Core temperature and pressure increase rapidly with mass, dramatically accelerating nuclear fusion rates.
Does this work for all stars?
Only for main-sequence (hydrogen-burning) stars. Giants, white dwarfs, and other evolved stars do not follow this relation.
What is the range of validity?
Roughly 0.08 to 150 M_sun. Below 0.08 M_sun, objects cannot sustain hydrogen fusion (brown dwarfs). Above 150 M_sun, the Eddington limit makes stars unstable.