Solar wind cross-helicity and residual energy during different solar cycles

Details Solar wind cross-helicity and residual energy during different solar cycles Solar wind cross-helicity and residual energy during different solar cycles

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsh41b1782p&link_type=abstract

American Geophysical Union, Fall Meeting 2010, abstract #SH41B-1782

Physics

Plasma Physics

[7536] Solar Physics, Astrophysics, And Astronomy / Solar Activity Cycle, [7863] Space Plasma Physics / Turbulence

Scientific paper

The minimum of solar cycle 23 exhibited anomalous characteristics with respect to its predecessors. Other than differences in the standard indicators of activity, such as sunspots, polar magnetic fields were also found to be different. These differences have a range of effects in the solar wind. In this work we investigate the behavior of the cross-helicity, i.e., the Alfvenicity, and of the residual energy, i.e., the balance between kinetic and magnetic energy, of the magnetic field fluctuations during two fast latitude scans from the solar minima in cycles 22 and 23 using Ulysses data. We find that the differences between the minima are mainly related to the greater prominence of convected structures in the broader equatorial region in cycle 23. For comparison, we have calculated the same parameters at different phases of the solar cycle and in a diverse range of solar wind regimes. We have found that the residual energy is independent of the phase of the solar cycle. We also highlight a dependence of cross-helicity and residual energy on different timescales from ~10 minutes to 10 hours.

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