Contribution of Solar Wind Dynamic Pressure Fluctuations to ULF Power in the Inner Magnetosphere

Details Contribution of Solar Wind Dynamic Pressure Fluctuations to ULF Power in the Inner Magnetosphere Contribution of Solar Wind Dynamic Pressure Fluctuations to ULF Power in the Inner Magnetosphere

May 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agusmsm42a..01t&link_type=abstract

American Geophysical Union, Fall Meeting 2007, abstract #SM42A-01

Physics

2724 Magnetopause And Boundary Layers, 2730 Magnetosphere: Inner, 2752 Mhd Waves And Instabilities (2149, 6050, 7836), 2784 Solar Wind/Magnetosphere Interactions, 2788 Magnetic Storms And Substorms (7954)

Scientific paper

We evaluate the contribution of the solar wind dynamic pressure fluctuations to magnetospheric magnetic field oscillations in the Pc5 band (1.6-6.7 mHz) using data from the ACE (solar wind) and GOES 8 (geostationary altitude) spacecraft and the CPMN ground stations (1 < L < 6) for 2001. In the first step of the analysis we compute band-integrated power (in hourly time windows) of oscillations of the solar wind dynamic pressure and the magnetic field in the magnetosphere and on the ground. In the second step we compute the correlation coefficient (CC) between log(dynamic pressure power) and log(magnetic field power). CC's calculated from the GOES 8 magnetic field magnitude and azimuthal component both exhibit a broad peak (CC ~ 0.7) around noon. CC's calculated from the ground H components exhibits a similar local time dependence, although the peak CC value decreases with increasing magnetic latitude. When the hourly mean of the solar wind velocity is used instead of the dynamic pressure oscillation power, the CC values are significantly lower at GOES and at low-latitude (L < 4) ground stations. These results suggest that the solar wind pressure oscillations are a dominant contributor to dayside magnetospheric ULF oscillations. The GOES observations indicate that varying solar wind dynamic pressure results in both compressional oscillations (Chapman-Ferraro current effect) and shear oscillations (mode conversion of compressional disturbances).

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