Other
Scientific paper
May 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agusmsm52a..03z&link_type=abstract
American Geophysical Union, Fall Meeting 2007, abstract #SM52A-03
Other
2720 Energetic Particles: Trapped, 2730 Magnetosphere: Inner, 2740 Magnetospheric Configuration And Dynamics, 2784 Solar Wind/Magnetosphere Interactions
Scientific paper
In this paper, we aim to study the long-term relativistic electron behavior in the often overlooked 'slot' region (l = 2-3) and the inner belt (l < 2) by using the daily-averaged 2-6 MeV electron fluxes obtained from the SAMPEX satellite during 1992-2003. In particular, we want to study the penetration of the MeV electrons at this energy range to the slot region and their flux enhancement in the inner belt and how these two processes are related to magnetospheric activity levels (such as Dst index) and some parameters in the solar wind (V, Pdyn, Nsw, Bz, B). It is found that the 2-6 Mev electron penetration usually takes place after those intense storms whose minimum Dst are less than -130 nT. For a total of 55 events meeting this Dst criterion, the penetration distance has a good correlation (r= 0.67) with the daily Dst minimum delayed by 3 days. But it has little or no correlation with any of the daily solar wind parameters. A superposed epoch analysis of 22 events based on another criterion (chosen when there is an obvious flux increase in the slot region at l = 2.5) reveals common characteristics in solar wind parameters and the Dst index associated with the penetration, with all reaching their peak values about 3 days prior to the flux peak in the slot region. Although the inner belt has fewer variations compared to the outer belt, it has its own response to different conditions. Analysis of the inner belt shows that the flux enhancement is directly associated with high solar wind speed (> 550 km/s) as well as low solar wind density (~4.4 cc). Either a couple of very extreme storms or recurrent intense storms will create conditions favorable for the MeV electron enhancement in the inner belt. However, without high speed solar wind on average, a large negative Dst alone is not a sufficient condition to create inner-belt electron flux enhancement.
Fok M.-
Li Xiaoliang
Lui A. T.
Zheng Yuanlin
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