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Taylor Microscale and Effective Reynolds Number near the Sun from PSP
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 ...
Phillips, C.; Bandyopadhyay, R.; McComas, D.~J.;
Published by: \apj Published on: jul
YEAR: 2022   DOI: 10.3847/1538-4357/ac713f
Parker Data Used; Solar wind; interplanetary turbulence; Magnetohydrodynamics; Space plasmas; 1534; 830; 1964; 1544; Astrophysics - Solar and Stellar Astrophysics; Physics - Space Physics