Dayside ionospheric response to the intense interplanetary shocks-solar wind discontinuities: Observations from the digisonde global ionospheric radio observatory

Details Dayside ionospheric response to the intense interplanetary shocks-solar wind discontinuities: Observations from the digisonde global ionospheric radio observatory Dayside ionospheric response to the intense interplanetary shocks-solar wind discontinuities: Observations from the digisonde global ionospheric radio observatory

Jun 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010jgra..11506304z&link_type=abstract

Journal of Geophysical Research, Volume 115, Issue A6, CiteID A06304

Physics

5

Ionosphere: Ionosphere/Magnetosphere Interactions (2736), Ionosphere: Electric Fields (2712), Interplanetary Physics: Interplanetary Shocks, Magnetospheric Physics: Magnetic Storms And Substorms (7954)

Scientific paper

The digisonde Global Ionospheric Radio Observatory (GIRO) has recorded strong ionospheric responses to two powerful interplanetary shock passages on 7 November 7 2004 and 21 January 2005. Both events provide excellent opportunities to study geospace response processes to strong interplanetary forward shocks in great detail. The angle between the normal of the 7 November 2004, shock front and the Sun-Earth line was ˜3.0 degrees, indicating that the shock hit the equatorial magnetosphere at ˜1200 LT (local noon). The subsequent dayside shock-induced ionospheric phenomena were found to have marked longitudinal and latitudinal distributions. Comparative studies of the intense interplanetary shocks (including the sheath) associated with northward and southward interplanetary magnetic fields (IMF) revealed their different geospace effects on the dayside ionospheric region. The equatorial ionosphere responds to the interplanetary shock rather quickly, and if the shock is associated with southward IMF the plasma electrons in the equatorial ionosphere are rapidly uplifted. During the 7 November 2004 event the averaged uplift velocity was close to ˜67 m/s, and the ionospheric total electron content (TEC) increased from the original 16 TEC units (TECU) to ˜38 TECU (1 TECU = 1016 m-2) which may be due to the shock effect. When the interplanetary shock (including the magnetosheath) is associated with northward IMF, the plasma in the equatorial ionosphere moves downward, causing a sudden drop in the total electron content. During the 21 January 2005 event, the averaged downward velocity was ˜120 m/s, and the TEC dropped from 75 TECU to 22 TECU at the time of maximum solar wind dynamic pressure, and then recovered to ˜68 TECU in about 2 h after the shock passage. The middle and high latitude ionospheric TEC enhancements may be due to particle (ion and electron) precipitation ionization losses caused by the strong impacts of the interplanetary shocks.

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