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Fig. 2


Contours of evaporation timescales (in yrs) of non-degenerate pulsar companions (tev,g and tev,c, Eqs. (17) and (21)) as a function of the companion radius R and its distance a to the pulsar in solar radii, for pulsar spin periods and magnetic fields as indicated (left to right: P = 1,10,100 ms and B = 108,108,1012 G), for conductivity times magnetic permeability σμ = 106s-1 and density ρ = 1 g cm-3. The white dotted line delimits the region where the cohesive energy dominates over gravitational energy (for small companions) for evaporation. The white region indicates evaporation times tev< 10 yr and yellow regions tev> 1012 yr.

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