Variation of Magnetospheric Dynamics During the Solar Cycle

Details Variation of Magnetospheric Dynamics During the Solar Cycle Variation of Magnetospheric Dynamics During the Solar Cycle

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agufmsh24a..05j&link_type=abstract

American Geophysical Union, Fall Meeting 2006, abstract #SH24A-05

Physics

Geophysics

2162 Solar Cycle Variations (7536), 2760 Plasma Convection (2463), 2784 Solar Wind/Magnetosphere Interactions, 4400 Nonlinear Geophysics (3200, 6944, 7839)

Scientific paper

Geomagnetic indices have been constructed to characterize/describe the magnetospheric state. Signatures of the solar cycle and the underlying solar wind/magnetospheric interaction are reflected in these indices. In order to study the long-term variability of magnetospheric dynamics, we have considered the nonlinear dependencies inherent to the Kp data stream from 1932-present. We find that the dynamics of the magnetosphere tend to be more linear at solar maximum than at solar minimum. The strong nonlinear dependencies tend to peak on a timescale around 40-50 hours and are statistically significant up to one week. Because the solar wind driver variables, VBs and dynamical pressure exhibit a much shorter decorrelation time for nonlinearities the results seem to indicate that the nonlinearity is related to internal magnetospheric dynamics. Moreover, the timescales for the nonlinearity seem to be on the same order as that for storm/ring current transport. In the descending phase of the solar cycle just prior to solar minimum, when magnetospheric activity is weaker, the dynamics exhibit a significant nonlinear internal magnetospheric response that appears to be related to increased solar wind speed. To investigate this effect further, we analyzed nonlinear dependencies during 1995-1996 when a series of high speed stream interfaces were detected in the solar wind, and we discuss the physical origin of the nonlinear response.

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