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Non-radial solar wind flows induced by the motion of interplanetary coronal mass ejections

By Mathew James Owens and P. Cargill

Abstract

A survey of the non-radial flows (NRFs) during\ud nearly five years of interplanetary observations revealed\ud the average non-radial speed of the solar wind flows to\ud be �30 km/s, with approximately one-half of the large\ud (>100 km/s) NRFs associated with ICMEs. Conversely, the\ud average non-radial flow speed upstream of all ICMEs is\ud �100 km/s, with just over one-third preceded by large NRFs.\ud These upstream flow deflections are analysed in the context\ud of the large-scale structure of the driving ICME. We chose\ud 5 magnetic clouds with relatively uncomplicated upstream\ud flow deflections. Using variance analysis it was possible to\ud infer the local axis orientation, and to qualitatively estimate the point of interception of the spacecraft with the ICME. For all 5 events the observed upstream flows were in agreement with the point of interception predicted by variance analysis. Thus we conclude that the upstream flow deflections in these events are in accord with the current concept of the large scale structure of an ICME: a curved axial loop connected to the Sun, bounded by a curved (though not necessarily circular)cross section

Publisher: European Geosciences Union
Year: 2004
OAI identifier: oai:centaur.reading.ac.uk:5838

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