Constraining Solar Wind Heating Processes by Kinetic Properties of Heavy Ions

Author
Keywords
Abstract
<p>We analyze the heavy ion components (A \&gt;4 amu ) in collisionally young solar wind plasma and show that there is a clear, stable dependence of temperature on mass, probably reflecting the conditions in the solar corona. We consider both linear and power law forms for the dependence and find that a simple linear fit of the form T<sub>i</sub>/T<sub>p</sub>=(1.35 \textpm.02 )m<sub>i</sub>/m<sub>p</sub> describes the observations twice as well as the equivalent best fit power law of the form T<sub>i</sub>/T<sub>p</sub>=(m<sup><sub>i</sub>/m<sub>p</sub>) 1.07 \textpm.01</sup> . Most importantly we find that current model predictions based on turbulent transport and kinetic dissipation are in agreement with observed nonthermal heating in intermediate collisional age plasma for m /q \&lt;3.5 , but are not in quantitative or qualitative agreement with the lowest collisional age results. These dependencies provide new constraints on the physics of ion heating in multispecies plasmas, along with predictions to be tested by the upcoming Solar Probe Plus and Solar Orbiter missions to the near-Sun environment</p>
Year of Publication
2016
Journal
Physical Review Letters
Volume
116303
Number
Number of Pages
255101
Date Published
06/2016
ISSN Number
0031-9007
URL
https://journals.aps.org/prl/abstract/10.1103/PhysRevLett.116.255101
DOI
10.1103/PhysRevLett.116.255101