Fig. 5
Comparison of different integration methods for a 2 M⊙ RG using the OPAL equation of state. The profile was cut at 5% of the stellar radius. Shown are the density ρ (upper left), the pressure p (upper right), the internal energy u (lower left), and the difference between the gradient ∇ and the adiabatic gradient ∇ad (lower right).
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