A turbulence-driven model for heating and acceleration of the fast wind in coronal holes
read the original abstract
A model is presented for generation of fast solar wind in coronal holes, relying on heating that is dominated by turbulent dissipation of MHD fluctuations transported upwards in the solar atmosphere. Scale-separated transport equations include large-scale fields, transverse Alfvenic fluctuations, and a small compressive dissipation due to parallel shears near the transition region. The model accounts for proton temperature, density, wind speed, and fluctuation amplitude as observed in remote sensing and in situ satellite data.
This paper has not been read by Pith yet.
Forward citations
Cited by 1 Pith paper
-
Radio Wave Propagation as a Probe of the Solar Corona and Solar Wind
Radio wave distortion effects serve as established probes of solar corona and wind turbulence parameters, with SKA expected to expand observational capabilities.
discussion (0)
Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.