Radius evolution (top panel) and evolutionary tracks in the H-R diagram (bottom) comparing the cold accretion (solid line) with the classical 1 M_⊙ evolution (dashed). The filled square indicates the initial location, the triangle indicates the stellar mass at 0.1 M_⊙, and the circle indicates the end of accretion. The non-accreting classical evolution, whose initial radius is assumed to be 4.92 R_⊙ as shown by the asterisks, starts at 0.99 × 10⁵ yr to compare the evolution. At 10⁵ yr, the radii are about one order of magnitude different. In the classical model the star evolves along the Hayashi and Henyey tracks, whereas in the cold accretion model the evolution is roughly horizontal in the H-R diagram. Although the deuterium burning slightly increases the luminosity where log T_eff ≃ 3.5, it is much smaller than the Henyey track of the non-accreting 1 M_⊙ star.