Dependence of the amplitude of Pc5-band magnetic field variations on the solar wind and solar activity

Details Dependence of the amplitude of Pc5-band magnetic field variations on the solar wind and solar activity Dependence of the amplitude of Pc5-band magnetic field variations on the solar wind and solar activity

Apr 2012

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012jgra..11704207t&link_type=abstract

Journal of Geophysical Research, Volume 117, Issue A4, CiteID A04207

Physics

Magnetospheric Physics: Magnetosphere: Inner, Magnetospheric Physics: Mhd Waves And Instabilities (2149, 6050, 7836), Magnetospheric Physics: Solar Wind/Magnetosphere Interactions

Scientific paper

We have studied the dependence of the amplitude of magnetic field variations in the Pc5 band (1.6–6.7 mHz) on the solar wind and solar activity. Solar wind parameters considered are the bulk velocity Vsw and the variation of the solar wind dynamic pressure δPsw. The solar activity dependence is examined by contrasting observations made in 2001 (solar activity maximum) and 2006 (solar activity declining phase). We calculated hourly Pc5 amplitude using data from geostationary satellites at L = 6.8 and ground stations covering 1 < L < 9. The amplitude is positively correlated with both Vsw and δPsw, but the degree of correlation varies with L and magnetic local time. As measured by the correlation coefficient, the amplitude dependence on both Vsw and δPsw is stronger on the dayside than on the nightside, and the dependence on Vsw (δPsw) tends to be stronger at higher (lower) L, with the relative importance of the two solar wind parameters switching at L ∼ 5. We attribute the Vsw control to the Kelvin-Helmholtz instability on the magnetopause, occurring both at high and low latitudes, and the δPsw control to buffeting of the magnetosphere by variation of solar wind dynamic pressure. The GOES amplitude is higher at the solar maximum at all local times and the same feature is seen on the ground in the dawn sector at L > 6. A radial shift of the fast mode wave turning point, associated with the solar cycle variation of magnetosphere mass density, is a possible cause of this solar activity dependence.

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