Dependence of the Occurrence of Low Latitude Pc3 Geomagnetic Pulsations on Solar Wind Velocity

Details Dependence of the Occurrence of Low Latitude Pc3 Geomagnetic Pulsations on Solar Wind Velocity Dependence of the Occurrence of Low Latitude Pc3 Geomagnetic Pulsations on Solar Wind Velocity

May 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agusmsm42a..02a&link_type=abstract

American Geophysical Union, Spring Meeting 2005, abstract #SM42A-02

Physics

0674 Signal Processing And Adaptive Antennas, 1555 Time Variations: Diurnal To Secular, 2164 Solar Wind Plasma, 2700 Magnetospheric Physics, 2784 Solar Wind/Magnetosphere Interactions

Scientific paper

Energy for the Earth's magnetospheric processes is provided by solar wind. Pc3 Geomagnetic pulsations are quasi-sinusoidal variations in the Earth's Magnetic field in the period range 10-45 seconds. The magnitude of these pulsations ranges from fraction of a nT(nano Tesla) to several nT. These pulsations can be observed in a number of ways. However the application of ground based manetometer arrays has proven to be one of the most successful methods of studying the spatial structure of hydromagnetic waves in the Earth's magnetosphere. With few exceptions, the Pc3 studies undertaken in the past have been confined to middle and high latitudes. The spatial and temporal variations observed in Pc3 occurrence are of vital importance because they provide evidence which can be directly related to wave generation mechanisms both inside and external to the magnetosphere. At low latitudes (L < 3) wave energy predominates in the Pc3 band and the spatial characteristics of these pulsations have received little attention in the past. An array of four low latitude induction coil magnetometers was established in south-east Australia over a longitudinal range of 17 degrees at L=1.8 to 2.7 for carrying out the study of the effect of the solar wind velocity on these pulsations. Digital dynamic spectra showing Pc3 pulsation activity over a period of about six months have been used to evaluate Pc3 pulsation occurrence. Pc3 occurrence probability at low latitudes has been found to be dominant for the solar wind velocity in the range 400-700 Km/sec. The results suggest that solar wind controls Pc3 occurrence through a mechanism in which Pc3 wave energy is convected through the magnetosheath and coupled to the standing oscillations of magnetospheric field lines.

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