Effect of solar wind velocity on magnetic cloud-associated magnetic storm intensity

Details Effect of solar wind velocity on magnetic cloud-associated magnetic storm intensity Effect of solar wind velocity on magnetic cloud-associated magnetic storm intensity

Nov 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002jgra..107.1346w&link_type=abstract

Journal of Geophysical Research (Space Physics), Volume 107, Issue A11, pp. SSH 3-1, CiteID 1346, DOI 10.1029/2002JA009396

Physics

19

Magnetospheric Physics: Storms And Substorms, Interplanetary Physics: Ejecta, Driver Gases, And Magnetic Clouds, Magnetospheric Physics: Solar Wind/Magnetosphere Interactions, Interplanetary Physics: Interplanetary Magnetic Fields

Scientific paper

We investigate geomagnetic storm activity during periods of 135 magnetic clouds identified with hourly averages of OMNI data from 1965 to 1998. It is found that the storm Dst index correlates well with both the Bz component (correlation coefficient, c.c. = -0.86) and the ``rectified'' electric field VBS (c.c. = -0.88) but does not correlate well with solar wind speed (c.c. = -0.58), indicating that the role of magnetic cloud speed in predicting storm intensity is a minor one. Solar wind speed does become important in predicting Dst for the studied cloud events when high solar wind speeds are considered. The correlation coefficient (c.c.) for Dst versus Bz increases dramatically when the solar wind speed exceeds 600 km/s. For example, the c.c. for Dst versus Bz is 0.99 for speeds between 600 and 750 km/s (15 events). This implies that solar wind velocity is also important indirectly for predicting the storm intensity when using Bz as a direct predictor. Specially, over the next 2 or 3 years, cloud speed is expected to increase, on average, as has already been observed. This provides us a good opportunity to estimate the intensity of cloud-associated geomagnetic storms by using the observed upstream Bz.

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