Automatic identification of magnetic clouds and cloud-like regions at 1 AU: occurrence rate and other properties

• Main Authors: R. P. Lepping, C.-C. Wu, D. B. Berdichevsky
• Format: Article
• Language: English
• Published: Copernicus Publications 2005-10-01
• Series: Annales Geophysicae
• Online Access: https://www.ann-geophys.net/23/2687/2005/angeo-23-2687-2005.pdf

A scheme is presented whose purpose is twofold: (1) to enable the automatic identification of an interplanetary magnetic cloud (MC) passing Earth from real-time measurements of solar wind magnetic field and plasma quantities or (2) for on-ground post-data collection MC identification ("detection" mode). In the real-time ("prediction") mode the scheme should be applicable to data from a spacecraft upstream of Earth, such as ACE, or to that of any near real-time field and plasma monitoring platform in the solar wind at/near 1AU. The initial identification of a candidate MC-complex is carried out by examining proton plasma beta, degree of small-scale smoothness of the magnetic field's directional change, duration of a candidate structure, thermal speed, and field strength. In a final stage, there is a test for large-scale B-field smoothness within the candidate regions that were identified in the first stage. The scheme was applied to WIND data over the period 1995 through mid-August of 2003 (i.e. over 8.6 years), in order to determine its effectiveness in identifying MC passages of any type (i.e. N<IMG WIDTH="19" HEIGHT="14" ALIGN="BOTTOM" BORDER="0" src="ag-23-2687-img1.gif" ALT="$Rightarrow$">S, S<IMG WIDTH="19" HEIGHT="14" ALIGN="BOTTOM" BORDER="0" src="ag-23-2687-img1.gif" ALT="$Rightarrow$">N, all S, all N, etc. types). (N<IMG WIDTH="19" HEIGHT="14" ALIGN="BOTTOM" BORDER="0" src="ag-23-2687-img1.gif" ALT="$Rightarrow$">S refers to the B<IMG WIDTH="13" HEIGHT="29" ALIGN="MIDDLE" BORDER="0" src="ag-23-2687-img2.gif" ALT="$_{Z}$"> component of the magnetic field going from north (+) to south (-) in GSE coordinates.) The distribution of these MC types for WIND is provided. The results of the scheme are compared to WIND MCs previously identified by visual inspection (called MFI MCs) with relatively good agreement, in the sense of capturing a large percentage of MFI MCs, but at the expense of finding a large percentage of "false positives". The scheme is shown to be able to find some previously ignored MCs among the false positives. It should be effective in helping to identify in real time most N<IMG WIDTH="19" HEIGHT="14" ALIGN="BOTTOM" BORDER="0" src="ag-23-2687-img1.gif" ALT="$Rightarrow$">S MCs for magnetic storm forecasting. The N<IMG WIDTH="19" HEIGHT="14" ALIGN="BOTTOM" BORDER="0" src="ag-23-2687-img1.gif" ALT="$Rightarrow$">S type of MC is expected to be most prevalent in solar cycle 24, which should start around 2007. The scheme is likely to be applicable to solar wind measurements taken well within 1 AU to well beyond it. <br><br><b>Keywords.</b> Interplanetary physics (Interplanetary magnetic fields; Solar wind plasma) – Magnetospheric physics (Solar wind-magnetosphere interactions)