Figure 1 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 1.

﹩{\mathrm{log}}_{10}({{\rm{\nabla }}}_{{\rm{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). As α_MLT decreases, the superadiabaticity ∇_s increases throughout the stellar interior, but ∇_s is inherently lower in main-sequence models.

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