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Long term observations by Brook et al. reveal that the derivative ofrotational frequency of PSR J0738-4042 changed abruptly in 2005. Originally,the spin-down rate was relatively stable, with the rotational frequencyderivative of $-1.14 \times 10^{-14}~\rm s^{-2}$. After September 2005, thederivative began to rise up. About 1000 days later, it arrived at anotherrelatively stable value of about $-0.98 \times 10^{-14}~\rm s^{-2}$, indicatingthat the pulsar is spinning-down relatively slowly. To explain the observedspin-down rate change, we resort to an asteroid disrupted by PSR J0738-4042. Inour model, the orbital angular momentum of the asteroid is assumed to beparallel to that of the rotating pulsar, so that the pronounced reduction inthe spin-down rate can be naturally explained as due to the transfer of theangular momentum from the disrupted material to the central pulsar. The derivedmagnetospheric radius is about $4.0 \times 10^{9}$ cm, which is smaller thanthe tidal disruption radius ($4.9 \times 10^{10}$ cm). Our model isself-consistent. It is shown that the variability of the spin-down rate of PSRJ0738-4042 can be quantitatively accounted for by the accretion from theasteroid disrupted by the central pulsar.

Reduced spin-down rate of PSR J0738-4042 explained as due to an asteroid disruption event