A Solar Coronal Hole and Fast Solar Wind Turbulence Model and First-orbit Parker Solar Probe (PSP) Observations
|Author||Adhikari, L.; Zank, G.; Zhao, L.-L.;|
|Keywords||Parker Data Used; parker solar probe; Solar Probe Plus|
We propose a turbulence-driven\ solar\ wind model for a fast\ solar\ wind flow in an open coronal hole where the\ solar\ wind flow and the magnetic field are highly aligned. We compare the numerical results of our model with\ Parker\ Solar\ Probe\ measurements of the fast\ solar\ wind flow and find good agreement between them. We find that (1) the majority quasi-2D turbulence is mainly responsible for coronal heating, raising the temperature to about similar to 1(6) K within a few\ solar\ radii, which leads in turn to the acceleration of the\ solar\ wind; (2) the heating rate due to quasi-2D turbulence near the coronal base is larger than that due to nearly incompressible/slab turbulence; (3) the quasi-2D energy in forward-propagating modes decreases with increasing distance, while the nearly incompressible/slab energy in forward-propagating modes increases, reaching a peak value at similar to 11.7 R-circle dot before decreasing with increasing heliocentric distance; (4) the correlation length increases with increasing distance from the coronal base; and (5) the variance of the density fluctuations decreases as a function of heliocentric distance.
|Year of Publication||2020|
|Journal||The Astrophysical Journal|
|Number of Pages||102|