Figure 3 from The Radius and Entropy of a Magnetized, Rotating, Fully Convective Star: Analysis with Depth-dependent Mixing Length Theories

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The Radius and Entropy of a Magnetized, Rotating, Fully Convective Star: Analysis with Depth-dependent Mixing Length Theories

Authors: Lewis G. Ireland, and Matthew K. Browning

2018 The Astrophysical Journal 856 132.

Provider: AAS Journals

Caption: Figure 3.

s as a function of log₁₀ (ρ) for 0.3 M_⊙, (a) 10 Myr or (b) 1 Gyr stellar models at α_MLT = 0.5–2.0 (Δ0.5). Decreasing α_MLT increases s_ad, i.e., the asymptotic value of specific entropy in the bulk of the convection zone, but to a lesser extent for main-sequence models.

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