  Turbulence in the Local Bubble could play an important role in the
thermodynamics of the gas that is there. The best astronomical technique for
measuring turbulence in astrophysical plasmas is radio scintillation.
Measurements of the level of scattering to the nearby pulsar B0950+08 by
Philips and Clegg in 1992 showed a markedly lower value for the line-of-sight
averaged turbulent intensity parameter $<C_N^2>$ than is observed for other
pulsars, consistent with radio wave propagation through a highly rarefied
plasma. In this paper, we discuss the observational progress that has been made
since that time. At present, there are four pulsars (B0950+08, B1133+16,
J0437-4715, and B0809+74) whose lines of sight seem to lie mainly within the
local bubble. The mean densities and line of sight components of the
interstellar magnetic field along these lines of sight are smaller than nominal
values for pulsars, but not by as much expected. Three of the four pulsars also
have measurements of interstellar scintillation. The value of the parameter
$<C_N^2>$ is smaller than normal for two of them, but is completely nominal for
the third. This inconclusive status of affairs could be improved by
measurements and analysis of ``arcs'' in ``secondary spectra'' of pulsars.
