Solar Wind Quasi-invariant for Slow and Fast Magnetic Clouds

Details Solar Wind Quasi-invariant for Slow and Fast Magnetic Clouds Solar Wind Quasi-invariant for Slow and Fast Magnetic Clouds

Apr 2012

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012soph..277..375w&link_type=abstract

Solar Physics, Volume 277, Issue 2, pp.375-388

Physics

Magnetic Clouds, Magnetic Storms, Quasi-Invariant, Solar Wind

Scientific paper

The solar wind quasi-invariant (QI) has been defined by Osherovich, Fainberg, and Stone ( Geophys. Res. Lett. 26, 2597, 1999) as the ratio of magnetic energy density and the energy density of the solar wind flow. In the regular solar wind QI is a rather small number, since the energy of the flow is almost two orders of magnitude greater than the magnetic energy. However, in magnetic clouds, QI is the order of unity (less than 1) and thus magnetic clouds can be viewed as a great anomaly in comparison with its value in the background solar wind. We study the duration, extent, and amplitude of this anomaly for two groups of isolated magnetic clouds: slow clouds (360< v<450 km s-1) and fast clouds (450≤ v<720 km s-1). By applying the technique of superposition of epochs to 12 slow and 12 fast clouds from the catalog of Richardson and Cane ( Solar Phys. 264, 189, 2010), we create an average slow cloud and an average fast cloud observed at 1 AU. From our analysis of these average clouds, we obtain cloud boundaries in both time and space as well as differences in QI amplitude and other parameters characterizing the solar wind state. Interplanetary magnetic clouds are known to cause major magnetic storms at the Earth, especially those clouds which travel from the sun to the Earth at high speeds. Characterizing each magnetic cloud by its QI value and extent may help in understanding the role of those disturbances in producing geomagnetic activity.

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