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The velocity and density distribution of $e^\pm$ in the pulsar wind arecrucial distinction among magnetosphere models, and contains key parametersdetermining the high energy emission of pulsar binaries. In this work, a directmethod is proposed, which might probe the properties of the wind from onepulsar in a double-pulsar binary. When the radio signals from the first-formedpulsar travel through the relativistic $e^\pm$ flow in the pulsar wind from theyounger companion, the components of different radio frequencies will bedispersed. It will introduce an additional frequency-dependent time-of-arrivaldelay of pulses, which is function of the orbital phase. In this paper, weformulate the above-mentioned dispersive delay with the properties of thepulsar wind. As examples, we apply the formula to the double pulsar system PSRJ0737-3039A/B and the pulsar-neutron star binary PSR B1913+16. For PSRJ0737-3039A/B, the time delay in 300\,MHz is $\lesssim10\mu$s near thesuperior-conjunction, under the optimal pulsar wind parameters, which is $\sim$half of the current timing accuracy. For PSR B1913+16, with the assumption thatthe neutron star companion has a typical spin down luminosity of$10^{33}$\,ergs/s, the time delay is as large as $10\sim20\mu$s in 300\,MHz.The best timing precision of this pulsar is $\sim5\mu$s in 1400\,MHz.Therefore, it is possible that we can find this signal in archival data.Otherwise, we can set an upper-limit on the spin down luminosity. Similaranalysis can be apply to other eleven known pulsar-neutron star binaries

monthly notices of the royal astronomical society

Probing the properties of the pulsar wind via studying the dispersive  effects in the pulses from the pulsar companion in a double neutron-star  binary system