  We place constraints on the properties of the interstellar turbulence that
surrounds Geminga pulsar, using the recent measurements from the HAWC
Observatory in this region. We propagate very-high-energy electrons in
realizations of 3D isotropic Kolmogorov or Kraichnan turbulence, calculate
their gamma-ray emission, and compare with HAWC measurements. We show that the
measurements can be well fitted for both models of the turbulence and for
reasonable values of its strength, $B_{\rm rms}$, and coherence length, $L_{\rm
c}$. Our best fits are obtained for $B_{\rm rms} \simeq 3 \mu$G and $L_{\rm c}
\simeq 1$ pc. Furthermore, the absence of strong asymmetries in the observed
emission favours $L_{\rm c} \leq 5$ pc.
