  Remarkable progress has been made in understanding turbulent astrophysical
plasmas in past decades including, notably, the solar wind and the interstellar
medium. In the case of the solar wind, much of this progress has relied on in
situ measurements from space-borne instruments. However, ground-based radio
observations also have played a significant role and have the potential to play
an even bigger role. In particular, using distant background sources (quasars,
pulsars, satellite beacons) to transilluminate the foreground corona and solar
wind, a variety of radio propagation phenomena can be used to map plasma
properties of the solar corona and heliosphere, as well as the warm
interstellar medium. These include angular broadening, interplanetary and
interstellar scintillations, and differential Faraday rotation. These
observations are highly complementary to in situ observations of the solar
wind, and could be a mainstay of investigations into turbulence of the ISM. We
point out that the Next Generation Very Large Array (ngVLA) fulfills all the
requirements necessary to exploit radio observations of astrophysical
turbulence fully.
