(a) A fluid element is displaced upward by inside a star and equilibrates in pressure…
PHYSICS · Subjective · Fermi University Physics · Astrophysics & Cosmology · Stellar structure, energy generation and evolution · Stellar structure, energy generation and evolution
Stars from the Inside, Ch Energy transport and the complete stellar model
Problem
(a) A fluid element is displaced upward by Δr>0 inside a star and equilibrates in pressure with its surroundings faster than it exchanges heat, so it evolves adiabatically. Its fractional density excess over the surroundings after the displacement is ρDρ=[δ(∇ad−∇)+φ∇μ]HPΔr, where δ≡−(∂lnρ/∂lnT)P>0, φ≡(∂lnρ/∂lnμ)P,T>0, ∇ is the local (surrounding) logarithmic temperature gradient, and ∇μ≡dlnμ/dlnP. A displaced element that ends up denser than its surroundings (Dρ>0) sinks back and the layer is stable. Derive the Ledoux criterion for convective stability, and show that it reduces to the Schwarzschild criterion when the composition is uniform. (b) Consider a family of stars supported by an ideal gas of mean molecular weight μ, in hydrostatic and thermal equilibrium, radiative throughout so ∇=∇rad everywhere, whose opacity follows a general power law κˉ=κ0ρaTb with constant exponents a and b. Using the homology assumption that all stars of this family have structurally similar ρ(r/R), T(r/R) profiles, so that central quantities scale as ρc∝M/R3, Pc∝GM2/R4 and Tc∝μPc/ρc, find how L scales with μ, M, R and κ0. Check that your result reproduces both homology relations of the text, and find the condition on a and b under which R drops out.