A nascent neutron star may be exposed to fallback accretion soon after theproto-neutron star stage. This high accretion episode can submerge the magneticfield deep in the crust. The diffusion of the magnetic field back to thesurface will take hundreds to millions of years depending on the amount of massaccreted and the consequent depth the field is buried. Neutron stars with largekick velocities will accrete less amount of fallback material leading toshallower submergence of their fields and shorter time-scales for the growth oftheir fields. We obtain the relation $\tau_{\rm Ohm} \propto v^{-1}$ betweenthe space velocity of the neutron star and Ohmic time-scale for the growth ofthe magnetic field. We compare this with the relation between the measuredtransverse velocities, $v_{\perp}$ and the field growth time-scales,$\mu/\dot{\mu}$, inferred from the measured braking indices. We find that theobservational data is consistent with the theoretical prediction though thesmall number of data precludes a strong conclusion. Measurement of thetransverse velocities of pulsars B1509$-$58, J1846$-$0258, J1119$-$6127 andJ1734$-$3333 would increase the number of the data and strongly contribute tounderstanding whether pulsar fields grow following fallback accretion.
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机译：初生中子星阶段后不久，新生中子星可能会暴露于后备增生。这种高吸积现象可能会将磁场浸没在地壳深处。磁场向表面的扩散将需要数百至数百万年的时间，具体取决于积聚的质量和磁场埋入的深度。速度大的中子星将积累较少的后备物质，从而导致其场的淹没程度更浅，并且场生长的时间尺度更短。对于磁场的增长，我们获得了中子星的空速和欧姆时标之间的关系$ \ tau _ {\ rm Ohm} \ propto v ^ {-1} $。我们将其与测得的横向速度$ v _ {\ perp} $和从测得的制动指数推断出的场生长时间尺度$ \ mu / \ dot {\ mu} $之间的关系进行比较。我们发现，观测数据与理论预测是一致的，尽管少量数据排除了有力的结论。脉冲星B1509 $-$ 58，J1846 $-$ 0258，J1119 $-$ 6127和J1734 $-$ 3333的横向速度的测量将增加数据的数量，并有助于理解脉冲场在回落积聚后是否会增长。
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