Dependence of geomagnetic activity during magnetic storms on the solar wind parameters for different types of streams: 3. Development of storm

Details Dependence of geomagnetic activity during magnetic storms on the solar wind parameters for different types of streams: 3. Development of storm Dependence of geomagnetic activity during magnetic storms on the solar wind parameters for different types of streams: 3. Development of storm

Feb 2012

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012ge%26ae..52...37n&link_type=abstract

Geomagnetism and Aeronomy, Volume 52, Issue 1, pp.37-48

Physics

Scientific paper

This paper is a continuation of (Nikolaeva et al., 2011, 2012) and it analyzes the development of the main phase of 190 magnetic storms with Dst ≤ -50 nT depending on the type of source in the solar wind (magnetic clouds, MC; corotating interaction regions, CIR; Ejecta; Sheath before them, ShE; Sheath before MC, ShMC; all Sheath regions before ICME, ShE + ShMC; all ICME, MC + Ejecta; and an indeterminate type of solar wind stream, IND). It is shown that at the main phase of all types of magnetic storms, the Dst index decreases with increasing integral electric field sumEy. The closeness of the relationship between these parameters (correlation coefficient) is higher for magnetic storms caused by Sheath before ICME than by MC and CIR. It is possible to assume that a high dynamic pressure intensifies the electric field effectiveness for four types of streams: Sheath (ShE, ShE + ShMC), CIR, and IND. Apparently, the Dst index does not depend on the IMF fluctuation level σ B for almost all types of streams (differences within error limits) against the background of the Dst dependence on sumEy of the main phase of a magnetic storm.

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