Characterization of solar wind driver gases causing intense geomagnetic storms

What is it about?

Classification and quantification of the interplanetary structures causing intense geomagnetic storms (Dst
100 nT) that occurred during 1997–2016 are studied. The subject of this consists of solar wind parameters of seventy-three intense storms that are associated with the southward interplanetary magnetic field. About 30.14% of the storms were driven by a combination of the sheath and ejecta (S + E), magnetic clouds (MC) and sheath field (S) are 26% each, 10.96% by combined sheath and MCs (S + C), while 5.48% of the storms were driven by ejecta (E) alone. Therefore, we want to aver that for storms driven by: (1) S + E. The Bz is high (10 nT), high density (q) (>10 N/cm3 ), high plasma beta (b) (>0.8), and unspecified (i.e. high or low) structure of the plasma temperature (T) and the flow speed (V); (2) MC. The Bz is 10 nT, low temperature (T
400,000 K), low q (
10 N/cm3 ), high V (450 km), and low b (
0.8); (3) The structures of S + C are similar to that of MC except that the V is low (V
450 km); (4) S. The Bz is high, low T, high q, unspecified V, and low b; and (5) E. Is when the structures are directly opposite of the one driven by MCs except for high V. Although, westward ring current indicates intense storms, but the large intensity of geomagnetic storms is determined by the intense nature of the electric field strength and the Bz. Therefore, great storms (i.e. Dst
200 nT) are manifestation of high electric field strength (13 mV/m).

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Why is it important?

It explained in detail the features of solar wind drivers leading to geomagnetic storms, a space weather event.