  As supernova remnants (SNRs) age, they become efficient cosmic ray
accelerators at their outer shell shocks. The current paradigm for shock
acceleration theory favors turbulent field environs in the proximity of these
shocks, turbulence driven by current instabilities involving energetic ions.
With the imminent prospect of dedicated X-ray polarimeters becoming a reality,
the possibility looms of probing turbulence on scales that couple to the
super-TeV electrons that emit X-rays. This paper presents model X-ray
polarization signatures from energetic electrons moving in simulated MHD
turbulence of varying levels of "chaos." The emission volumes are finite slabs
that represent the active regions of young SNR shells. We find that the
turbulent field energy must be quite limited relative to that of the total
field in order for the X-ray polarization degree to be as strong as the radio
measures obtained in some remnants. Results presented are pertinent to the
planned IXPE and XIPE polarimeters.
