Physics
Scientific paper
Dec 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsa44a..08s&link_type=abstract
American Geophysical Union, Fall Meeting 2011, abstract #SA44A-08
Physics
[2772] Magnetospheric Physics / Plasma Waves And Instabilities, [2774] Magnetospheric Physics / Radiation Belts, [2784] Magnetospheric Physics / Solar Wind/Magnetosphere Interactions, [2788] Magnetospheric Physics / Magnetic Storms And Substorms
Scientific paper
One of the major outstanding scientific problems in the field of heliophysics is understanding and quantifying the dominant source and loss processes that contribute to the variability of relativistic electron populations in the Earth's outer radiation belt. It is known that the dynamics of the outer belt is highly dependent on the driving solar wind conditions during and in the aftermath of geomagnetic storms. For example, geomagnetic storms driven by corotating interaction regions (CIRs) and the following high speed stream (HSS) are particularly efficient at coupling energy into the magnetosphere. Despite the fact that CIR/HSS-driven storms have on average a weaker Dst signature than storms driven by coronal mass ejections (CMEs), these storms typically result in significant outer belt flux enhancements. One process that is believed to play a major role in the evolution of the outer belt is cyclotron-resonant wave particle interactions involving whistler-mode chorus emissions. Chorus interactions can result in the precipitative loss of electrons over a wide range of energy as well as the acceleration of seed electrons (10's to 100's of keV) up to energies of an MeV or greater. Progress in quantifying the role of chorus in radiation belt dynamics requires knowledge of how the chorus wave power varies with time and space as a function of solar wind and magnetospheric conditions. While in situ measurements of chorus are relatively sparse during solar cycle 23, a large database of ground-based ELF/VLF observations from Antarctica exist for this period. Here we examine the variation of chorus activity observed on the ground during a set of geomagnetic storms from 2000 to 2010. We analyze data from Palmer Station, Antarctica (Λ=-50o) and South Pole Station, Antarctica (Λ=-74o) thus covering waves generated in the inner magnetosphere as well as in the dayside outer magnetosphere. We explore differences in the intensity, duration and spectral extent of chorus between CIR/HSS-driven storms and CME-driven storms, and we put the results in the context of the global magnetospheric response such as differences in substorm activity and plasmasheet density and temperature.
Golden D. I.
Spasojevic Maria
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