Fig. 1.
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Initial stratification in the problem units (Table 1) of the pressure p, density ρ, pseudo-entropy A = p/ργ, and mean molecular weight μ in the stellar model (thin lines) and in the test problem (thick lines). The discontinuity visible in the stellar model at r ≈ 2.35 is the bottom of the carbon-burning shell, which is not included in our test problem.
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