Magnetic Reconnection May Control the Ion-scale Spectral Break of Solar Wind Turbulence
AffiliationUniv Arizona, Lunar & Planetary Lab
MetadataShow full item record
CitationDaniel Vech et al 2018 ApJL 855 L27
Rights© 2018. The American Astronomical Society.
Collection InformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at firstname.lastname@example.org.
AbstractThe power spectral density of magnetic fluctuations in the solar wind exhibits several power-law-like frequency ranges with a well-defined break between approximately 0.1 and 1 Hz in the spacecraft frame. The exact dependence of this break scale on solar wind parameters has been extensively studied but is not yet fully understood. Recent studies have suggested that reconnection may induce a break in the spectrum at a “disruption scale” lD, which may be larger than the fundamental ion kinetic scales, producing an unusually steep spectrum just below the break. We present a statistical investigation of the dependence of the break scale on the proton gyroradius ρi, ion inertial length di, ion sound radius ρs, proton–cyclotron resonance scale ρc, and disruption scale lD as a function of b^i. We find that the steepest spectral indices of the dissipation range occur when βe is in the range of 0.1–1 and the break scale is only slightly larger than the ion sound scale (a situation occurring 41% of the time at 1 au), in qualitative agreement with the reconnection model. In this range, the break scale shows a remarkably good correlation with lD. Our findings suggest that, at least at low βe, reconnection may play an important role in the development of the dissipation range turbulent cascade and cause unusually steep (steeper than −3) spectral indices.
NoteOpen access article.
VersionFinal Published Version