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Table 1

Gravitational (tev,g) and cohesive (tev,c) evaporation timescales due to induction heating for various pulsar and companion parameters.

System R a P B x Qabs tev,c tev,g tev,c tev,g
[km] [R] [ms] [108G] [yr] (ρσ = 106 s-1) [yr] (ρσ = 107 s-1)

bodies very 1. 1. 1. 1. 0.003 3. × 10-5 20. (2. × 10-6) 0.6 (7. × 10-8)
near 1 ms 102 1. 1. 1. 0.33 9. × 10-2 0.6 (0.007) 6 (0.007)
pulsar 103 1. 1. 1. 3.3 0.11 5.5 (0.6) 54 (6.)

asteroid 1. 1. 10. 1. 3. × 10-4 3. × 10-7 2. × 107 (2.) 6. × 105 (0.06)
and 10 ms PSR 1. 200. 10. 1. 3. × 10-4 3. × 10-7 8. × 1011 (9. × 104) 8. × 1011 (9. × 104)

asteroid + 1 s PSR 1. 1. 103 104 3. × 10-6 3. × 10-11 2. × 1011 (2. × 104) 2.4 × 1010 (2.7 × 103)

asteroid + PSR 1931+24 1. 0.14 813. 104 4. × 10-6 5. × 10-11 1.1 × 109 (128) 6. × 109 (683)

PSR 1257+12a 1800. 42. 6. 8.8 1. 0.06 5. × 105 (1.7 × 105) 4. × 106 1.7 × 106
PSR 1257+12b 104 77. 6. 8.8 5.5 0.04 (1.5 × 107) 1.6 × 108 1.5 × 108 1.6 × 109
PSR 1257+12c 104 98. 6. 8.8 5.5 0.04 (2.3 × 107) 2.6 × 108 (2.3 × 108) 2.6 × 109

Notes. We assume a mass density ρ = 3 g cm-3 and μσ = 106,107 s-1 for Cols. 8, 9 and 10, 11, respectively. Values of Qabs were computed with Damie. Timescale values in parentheses are only indicative as the other timescale dominates the evaporation regime.

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