Photospheric evolution in the density‐temperature plane. The evolutionary sequences are plotted on top of the hydrogen‐rich opacity table. Darker shades of gray represent higher opacities. The size of the open circle representing a converged model is in proportion to the actual radius of the star. The stars begin their evolution on the Hayashi track, clustered fairly close together near the point log₁₀T ≈ 3.3, log₁₀ρ ≈ −5.5. Notice that the M_* = 0.08 model slides all the way along the grain opacity boundary to a photospheric density log₁₀ρ ≈ −5.5 before reaching the main sequence.