Evolution of MSs of various masses to WDs in H-R diagrams, where L is the luminosity and T_e the effective temperature of the star. The solid, dashed, and long-dashed lines show the evolution from MS to WD without accretion, from bottom to top: for 3,  5, and 8 M_⊙ MSs. Accretion at ﹩\dot{M}=1{0}^{-9}\,{M}_{\odot }\,{{\rm{yr}}}^{-1}﹩ onto the 1.02 M_⊙ WD with an initially dormant magnetic field leads to a 2.4 M_⊙ B-WD (dotted line), whereas without a magnetic field, a M_Ch = 1.4 M_⊙ WD forms (dash–dotted line). The magnetic evolution is done as per the route described in the Appendix B with magnetic field parameters η = 1.3, γ = 0.9.