Determine the scaling of the luminosity L with M and R for (a) a low– mass star and (b) a high–mass star.
By the principle of homology, a temperature increment dT scales in the same way as T, which eqn 35.58 gives as T(r) ∝ MR^{−1}. An increment in radius, however, scales with radius, i.e. dR ∝ R. Therefore the temperature gradient follows dT/dr ∝ MR^{−1}/R, giving
\frac{dT}{dr} ∝ MR^{−2} . (35.61)
Equation 35.45 becomes
\frac{dT}{dr} = -\frac{3κ(r)ρ(r)L(r) }{64πr^{2} σ[T(r)]^{3} } (35.45)
\frac{L(r) }{r^{2} }∝ − \frac{T(r)^{ 3} }{ρ(r)κ(r)} \frac{dT}{dr}, (35.62)
and hence in case (a), for which κ(r) ∝ ρ(r)T(r)^{ -3.5}, we find
L(r) ∝ \frac{M^{5.5} }{R^{0.5} }. (35.63)
The assumption of homology means that if the luminosity at any radius r scales as M^{5.5}R^{-0.5}, then the surface luminosity scales in this way, so we may write
L ∝ \frac{M^{5.5} }{R^{0.5} }. (35.64)
For case (b), since κ(r) is a constant, we find L(r) ∝ M³ and hence
L ∝ M³. (35.65)