  CONTEXT. Hydrodynamical cosmological simulations predict flows of the
intergalactic medium along the radial vector of the voids, approximately in the
direction of the infall of matter at the early stages of the galaxy formation.
  AIMS. These flows might be detected by analysing the dependence of the warp
amplitude on the inclination of the galaxies at the shells of the voids with
respect to the radial vector of the voids. This analysis will be the topic of
this paper.
  METHODS. We develop a statistical method of analysing the correlation of the
amplitude of the warp and the inclination of the galaxy at the void surface.
This is applied to a sample of 97 edge-on galaxies from the Sloan Digital Sky
Survey. Our results are compared with the theoretical expectations, which are
also derived in this paper.
  RESULTS. Our results allow us to reject the null hypothesis (i.e., the
non-correlation of the warp amplitude and the inclination of the galaxy with
respect to the void surface) at 94.4% C. L., which is not conclusive. The
absence of the radial flows cannot be excluded at present, although we can put
a constraint on the maximum average density of baryonic matter of the radial
flows of <rho_b> <~ 4 Omega_b rho_crit.
