Strong Preferential Ion Heating is Limited to within the Solar Alfvén Surface
AffiliationUniv Arizona, Lunar & Planetary Lab
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PublisherIOP PUBLISHING LTD
CitationKasper, J. C., & Klein, K. G. (2019). Strong Preferential Ion Heating is Limited to within the Solar Alfvén Surface. The Astrophysical Journal Letters, 877(2), L35.
JournalASTROPHYSICAL JOURNAL LETTERS
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AbstractThe decay of the solar wind helium-to-hydrogen temperature ratio due to Coulomb thermalization can be used to measure how far from the Sun strong preferential ion heating occurs. Previous work has shown that a zone of preferential ion heating, resulting in mass-proportional temperatures, extends about 20-40 R-circle dot from the Sun on average. Here we look at the motion of the outer boundary of this zone with time and compare it to other physically meaningful distances. We report that the boundary moves in lockstep with the Alfven point over the solar cycle, contracting and expanding with solar activity with a correlation coefficient of better than 0.95 and with an rms difference of 4.23 R-circle dot. Strong preferential ion heating is apparently predominately active below the Alfven surface. To definitively identify the underlying preferential heating mechanisms, it will be necessary to make in situ measurements of the local plasma conditions below the Alfven surface. We predict that the Parker Solar Probe (PSP) will be the first spacecraft to directly observe this heating in action, but only a couple of years after launch as activity increases, the zone expands, and PSP's perihelion drops.
NoteOpen access article
VersionFinal published version
SponsorsWind grant [NNX14AR78G]; NASA HSR grant [NNX16AM23G]