Redshifted temperature as a function of mass density inside neutron stars with B = 0 (solid lines), 10¹⁵ G (long-dashed and dotted lines), and 10¹⁶ G (dot-dashed lines) at four ages t from 8 h to 2 × 10⁴ yr, marked near the curves. The dotted line illustrates the model with superfluidity SF081322; the other lines are calculated without superfluidity. The two parts of the figure, separated by the vertical solid line, show the regions before and after neutron drip at different density scales. Inset: temperature profiles in the envelopes of a neutron star with B = 10¹⁴ G at ages t = 1, 5, 20, and 100 kyr.