  We evaluate the prospects for radio follow-up of the double neutron stars
(DNSs) in the Galactic disk that could be detected through future space-borne
gravitational wave (GW) detectors. We first simulate the DNS population in the
Galactic disk that is accessible to space-borne GW detectors according to the
merger rate from recent LIGO results. Using the inspiraling waveform for the
eccentric binary, the average number of the DNSs detectable by TianQin (TQ),
LISA, and TQ+LISA are 217, 368, and 429, respectively. For the joint GW
detection of TQ+LISA, the forecasted parameter estimation accuracies, based on
the Fisher information matrix, for the detectable sources can reach the levels
of $\Delta P_{\mathrm b}/P_{\mathrm b} \lesssim 10^{-6}$, $\Delta \Omega
\lesssim 100~{\mathrm {deg}}^2$, $\Delta e/e \lesssim 0.3$, and $\Delta
\dot{P}_{\mathrm b} / \dot{P}_{\mathrm b} \lesssim 0.02$. These estimation
accuracies are fitted in the form of power-law function of signal-to-noise
ratio. Next, we simulate the radio pulse emission from the possible pulsars in
these DNSs according to pulsar beam geometry and the empirical distributions of
spin period and luminosity. For the DNSs detectable by TQ+LISA, the average
number of DNSs detectable by the follow-up pulsar searches using the Parkes,
FAST, SKA1, and SKA are 8, 10, 43, and 87, respectively. Depending on the radio
telescope, the average distances of these GW-detectable pulsar binaries vary
from 1 to 7 kpc. Considering the dominant radiometer noise and phase jitter
noise, the timing accuracy of these GW-detectable pulsars can be as low as 70
${\rm ns}$ while the most probable value is about 100 $\mu {\rm s}$.
