Neutrino emission power density as a function of mass density at ages 50 yr (upper curves) and 5 kyr (lower curves of each type) for nonsuperfluid magnetars with B = 10¹⁴ G (short-dashed lines), 10¹⁵ G (long-dashed lines), and 10¹⁶ G (dot-dashed lines) and for a magnetar with B = 10¹⁵ G and nucleon superfluidity (dotted lines), compared with neutrino emission of a nonmagnetic, nonsuperfluid neutron star (solid lines). The density scale is different in the left and right parts of the figure, separated by the vertical solid line. The vertical dotted lines mark the outer and inner boundaries of the inner crust.