Varying the angular momentum accretion history, for Ṁ = 10^-3M_⊙ yr^-1. Upper panel: internal structure of the non-rotating model: the upper curve is the stellar radius, the dark grey regions are convective, the light grey is radiative, and the dotted lines are ios-mass of 2, 4, 6, 8,..., M_⊙. Second panel: three J-accretion histories considered and the third one, specifically, shows the evolution of v_surf/v_crit for the corresponding models (the grey dotted horizontal line indicates the critical limit), and bottom panel: deformation of the star due to rotation (R_eq and R_pol are the equatorial and polar radii, respectively).