Relationship of solar wind parameters to dayside equatorial Pc4 pulsations

Details Relationship of solar wind parameters to dayside equatorial Pc4 pulsations Relationship of solar wind parameters to dayside equatorial Pc4 pulsations

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsa51d1973c&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #SA51D-1973

Physics

[2752] Magnetospheric Physics / Mhd Waves And Instabilities, [2784] Magnetospheric Physics / Solar Wind/Magnetosphere Interactions

Scientific paper

The results from early and recent observations have shown that Pc4 pulsations are influenced by solar wind parameters. Their sources are either upstream waves generated by ion-cyclotron instability or surface waves by Kelvin-Helmholtz instability (KHI). Most studies on Pc4 pulsations have analyzed data from satellites and high-latitude ground stations. Thus, in this paper, we present the results of a statistical study of Pc4 pulsations observed at equatorial MAGDAS/CPMN stations. Our analysis shows that the occurrence and amplitude of equatorial Pc4 pulsations have local time dependence. The maximum occurrence and maximum amplitude occur during daytime. The comparison between Pc4 amplitude and the IMF cone angle shows very little correlation, which suggests that the possibility of upstream waves as the main source may not be considered. We find a strong correlation between the Pc4 amplitude and the solar wind speed and variation of dynamic pressure as well. Since we didn't observe any strong Pc4 activity at dawn and dusk, the KHI mechanism cannot explain this type of equatorial Pc4 pulsation. A possible mechanism is the velocity shear instability in the magnetosphere boundary layers, which generates localized HM waves (Yumoto, 1984).

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