Recovery phase of magnetic storms induced by different interplanetary drivers

Abstract

Statistical analysis of Dst behaviour during recovery phase of magnetic storms induced by different types of interplanetary drivers is made on the basis of OMNI data in period 1976-2000. We study storms induced by ICMEs (including magnetic clouds (MC) and Ejecta) and both types of compressed regions: corotating interaction regions (CIR) and Sheaths. The shortest, moderate and longest durations of recovery phase are observed in ICME-, CIR-, and Sheath-induced storms, respectively. Recovery phases of strong ($Ds{t}_{min}<-100$ nT) magnetic storms are well approximated by hyperbolic functions $Dst(t)=a/(1+t/{\tau }_h)$ with constant ${\tau }_h$ times for all types of drivers while for moderate ($-100<Ds{t}_{min}<-50$ nT) storms $Dst$ profile can not be approximated by hyperbolic function with constant ${\tau }_h$ because hyperbolic time ${\tau }_h$ increases with increasing time of recovery phase. Relation between duration and value $Ds{t}_{min}$ for storms induced by ICME and Sheath has 2 parts: $Ds{t}_{min}$ and duration correlate at small durations while they anticorrelate at large durations.

18 pages, 4 figures, 2 tables, submitted to JGR special issue "Response of Geospace to High-Speed Streams"

References in corpus (2)

• Geoeffectiveness and efficiency of CIR, Sheath and ICME in generation of magnetic storms
• A Hyperbolic Decay of the Dst Index during the Recovery Phase of Intense Geomagnetic Storms

Cited by in corpus (3)

• Age dependence of wind properties for solar type stars: a 3d study
• Influence of the interplanetary driver type on the durations of main and recovery phases of magnetic storms
• Whether duration of the recovery phase of magnetic storm depends on the development rate of storm at its main phase?