Interplanetary magnetic cloud trigging locations of magnetic storm occurrences

Details Interplanetary magnetic cloud trigging locations of magnetic storm occurrences Interplanetary magnetic cloud trigging locations of magnetic storm occurrences

May 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agusm..sh22c10w&link_type=abstract

American Geophysical Union, Spring Meeting 2001, abstract #SH22C-10

Physics

2788 Storms And Substorms, 7524 Magnetic Fields, 7599 General Or Miscellaneous, 7851 Shock Waves

Scientific paper

The authors will investigate geomagnetic activity which was associated with magnetic cloud events and also study some aspects of the cloud's magnetic field structure (e.g., magnetic field distribution of the cloud). Thirty four magnetic cloud events observed by WIND over the years 1995, 1996 and 1997, and very early 1998 will be investigated in this study. Magnetic clouds are usually a dramatic source of long-lasting, strong, interplanetary, negative Bz fields (in solar magnetospheric coordinates) and are known to be a major source of geomagnetic activity (Dst < -50~nT). The region just upstream of a cloud may be a significant source of southward fields instead of, or as well as, the cloud itself. We call this upstream region a ``sheath" if it is bounded by a shock (or a pressure pulse) and the cloud. This study will help to identify the major sources (regions of initial Bz turning following shock passages or within the magnetic clouds) which are most dominant in the generation of geomagnetic storms. It was found that a geomagnetic storm could be induced by (i) a sheath, (ii) the front region of a cloud, (iii) the ends of a cloud, and (iv) both regions, sheath and cloud. (Because of this complexity, multiple storms can occur.) The related occurrence percentages of storms were 17.6%, 44.1%, 20.6%, and 5.9%, and the averaged storm sizes (minimum Dst) were -60, -85, -92, and -58~nT, respectively. The occurrence percentage of ``no-storm" cases (i.e., Dst < -30~nT) was 11.8%.

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