Main-Sequence Mass-Luminosity Relation

What you are seeing: the steep dependence of stellar luminosity on mass on the main sequence, approximated by piecewise power laws. A 2 $M_\odot$ star is $\sim 16 \times$ brighter than the Sun; a 10 $M_\odot$ star is $\sim 5000 \times$ brighter. Lifetime scales as $M / L$ .

Figure 1.

L(M)

on the main sequence.

M / M⊙1.0

WHAT TO TRY

Slide the mass up: luminosity climbs far faster (roughly L ~ M^3.5), so a 10 solar-mass star is thousands of times brighter than the Sun. Small mass changes mean huge luminosity changes.
Note the lifetime scaling M/L: massive stars burn through their fuel fast and die young despite having more of it. A 10 solar-mass star lives a thousand times shorter than the Sun.
Watch the piecewise power law bend: the exponent shifts across mass regimes as the dominant opacity and energy transport change.