A Solar Coronal Hole and Fast Solar Wind Turbulence Model and First-orbit Parker Solar Probe (PSP) Observations

Author
Keywords
Abstract
<p>We propose a turbulence-driven\&nbsp;solar\&nbsp;wind model for a fast\&nbsp;solar\&nbsp;wind flow in an open coronal hole where the\&nbsp;solar\&nbsp;wind flow and the magnetic field are highly aligned. We compare the numerical results of our model with\&nbsp;Parker\&nbsp;Solar\&nbsp;Probe\&nbsp;measurements of the fast\&nbsp;solar\&nbsp;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\&nbsp;solar\&nbsp;radii, which leads in turn to the acceleration of the\&nbsp;solar\&nbsp;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.</p>
Year of Publication
2020
Journal
The Astrophysical Journal
Volume
901
Number
Number of Pages
102
Date Published
10/2020
URL
https://iopscience.iop.org/article/10.3847/1538-4357/abb132https://iopscience.iop.org/article/10.3847/1538-4357/abb132/pdf
DOI
10.3847/1538-4357/abb132