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Substorm dependence of plasmaspheric hiss

By N.P. Meredith, R.B. Horne, R.M. Thorne, D. Summers and R.R. Anderson


We analyze wave and particle data from the CRRES satellite to determine the variability of plasmaspheric hiss (0.1 < f < 2 kHz) with respect to substorm activity as measured by AE*, defined as the maximum value of the AE index in the previous 3 hours. The study is relevant to modeling the acceleration and loss of relativistic electrons during storms and understanding the origin of the waves. The plasmaspheric hiss amplitudes depend on spatial location and susbtorm activity, with the largest waves being observed during high levels of substorm activity. Our survey of the global distribution of hiss indicates a strong day-night asymmetry with two distinct latitudinal zones of peak wave activity primarily on the dayside. Equatorial hiss (\lambda(m)\ < 15 degrees) is strongest during active conditions (AE* > 500 nT), with an average amplitude of 40 +/- 1 pT observed in the region 2 < L < 4 from 0600 to 2100 MLT. Midlatitude (\lambda(m)\ > 15degrees) hiss is strongest during active conditions with an average amplitude of 47 +/- 2 pT in the region 2 < L < 4 from 0800 to 1800 MLT but extending out beyond L = 6 from 1200 to 1500 MLT. Equatorial hiss at 600 Hz has minimum cyclotron resonant energies ranging from similar to20 keV at L = 6 to similar to1 MeV at L = 2, whereas midlatitude hiss at 600 Hz has minimum resonant energies ranging from similar to50 keV at L = 6 to similar to2 MeV at L = 2. The enhanced equatorial and midlatitude hiss emissions are associated with electron flux enhancements in the energy range of tens to hundreds of keV, suggesting that these electrons are the most likely source of plasmaspheric hiss. The enhanced levels of plasmaspheric hiss during substorm activity will lead to increased pitch-angle scattering of energetic electrons and may play an important role in relativistic electron dynamics during storms

Topics: Meteorology and Climatology, Physics, Atmospheric Sciences
Publisher: American Geophysical Union
Year: 2004
DOI identifier: 10.1029/2004JA010387
OAI identifier:
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