  The Taylor microscale is a fundamental length scale in turbulent fluids,
representing the end of fluid properties and onset of dissipative processes.
The Taylor microscale can also be used to evaluate the Reynolds number in
classical turbulence theory. Although the solar wind is weakly collisional, it
approximately behaves as a magnetohydrodynamic (MHD) fluid at scales larger
than the kinetic scale. As a result, classical fluid turbulence theory and
formalisms are often used to study turbulence in the MHD range. Therefore, a
Taylor microscale can be used to estimate an effective Reynolds number in the
solar wind. NASA's Parker Solar Probe (PSP) has reached progressively closer to
the Sun than any other spacecraft before. The collected data have revealed many
new findings in the near-Sun solar wind. Here, we use the PSP data to estimate
the Taylor microscale and effective Reynolds number near the Sun. We find that
the Taylor microscale and Reynolds number are small compared to the
corresponding near-Earth values, indicating a solar wind that has been less
processed by turbulence, with very small-scale dissipative processes near the
Sun.
