In the convective core of a massive main-sequence star the local values are , , , ,

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

In the convective core of a massive main-sequence star the local values are ρ=6.0×103 kg m−3\rho = 6.0\times10^{3}\,\mathrm{kg\,m^{-3}}, cP=1.5×104 J kg−1 K−1c_P = 1.5\times10^{4}\,\mathrm{J\,kg^{-1}\,K^{-1}}, T=3.0×107 KT = 3.0\times10^{7}\,\mathrm{K}, g=4.0×103 m s−2g = 4.0\times10^{3}\,\mathrm{m\,s^{-2}}, δ=1\delta=1, pressure scale height HP=1.0×108 mH_P = 1.0\times10^{8}\,\mathrm{m}, mixing length ℓ=1.8×108 m\ell = 1.8\times10^{8}\,\mathrm{m}, and superadiabatic excess ∇−∇ad=1.0×10−8\nabla-\nabla_{\rm ad} = 1.0\times10^{-8}. Use Fconv≈ρcPTgδ ℓ242HP−3/2(∇−∇ad)3/2F_{\rm conv} \approx \rho c_P T\sqrt{g\delta}\,\frac{\ell^2}{4\sqrt2}H_P^{-3/2}(\nabla-\nabla_{\rm ad})^{3/2} to estimate the convective flux FconvF_{\rm conv} carried at this point.

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