Temporal evolution of the masses (M, top row), radii (R, second row), loss-cone (﹩{\dot{N}}_{{\rm{lc}}}﹩, third row), and evaporation rates (﹩{\dot{N}}_{{\rm{ev}}}﹩, bottom row) while varying the seed mass of the central growing BH (black lines, top row). We assume stars and stellar-mass BHs have the same inner cusp slopes α₁ = α₂, and different columns consider different index values: α₁ = 0 (left column), α₁ = −0.5 (second column), α₁ = −1.0 (third column), and α₁ = −1.5 (right column). All other parameters of the model have been fixed. Here Q is the ratio of total mass in stellar-mass BHs (m₂ = 10 M_⊙) to the total mass in low-mass stars (m₁ = 1 M_⊙).