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Published February 2009 | Published + Supplemental Material
Journal Article Open

Multispacecraft Observations of Magnetic Clouds and Their Solar Origins between 19 and 23 May 2007

Abstract

We analyze a series of complex interplanetary events and their solar origins that occurred between 19 and 23 May 2007 using observations by the STEREO and Wind satellites. The analyses demonstrate the new opportunities offered by the STEREO multispacecraft configuration for diagnosing the structure of in situ events and relating them to their solar sources. The investigated period was characterized by two high-speed solar wind streams and magnetic clouds observed in the vicinity of the sector boundary. The observing satellites were separated by a longitudinal distance comparable to the typical radial extent of magnetic clouds at 1 AU (fraction of an AU), and, indeed, clear differences were evident in the records from these spacecraft. Two partial-halo coronal mass ejections (CMEs) were launched from the same active region less than a day apart, the first on 19 May and the second on 20 May 2007. The clear signatures of the magnetic cloud associated with the first CME were observed by STEREO B and Wind while only STEREO A recorded clear signatures of the magnetic cloud associated with the latter CME. Both magnetic clouds appeared to have interacted strongly with the ambient solar wind and the data showed evidence that they were a part of the coronal streamer belt. Wind and STEREO B also recorded a shocklike disturbance propagating inside a magnetic cloud that compressed the field and plasma at the cloud's trailing portion. The results illustrate how distant multisatellite observations can reveal the complex structure of the extension of the coronal streamer into interplanetary space even during the solar activity minimum.

Additional Information

© The Author(s) 2009. This article is published with open access at Springerlink.com. 24 June 2008 Accepted: 25 November 2008 Published online: 20 December 2008. Work at the University of California, Berkeley, was supported from STEREO Grant No. NAS5-03131. C. Möstl acknowledges funding from the Steiermärkische Sparkasse and by the Austrian FWF project P20145-N16. C. Farrugia acknowledges NASA Grant Nos. NNX08AD11G and NNG06GD41G. Antoinette Galvin acknowledges NASA Contract No. NAS5-00132. The SECCHI data used here were produced by an international consortium of the NRL (USA), LMSAL (USA), NASA/GSFC (USA), RAL (UK), MPS (Germany), CSL (Belgium), IOTA (France), and IAS (France). The work of P.C. Liewer was performed at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. This work utilizes data obtained by the Global Oscillation Network Group (GONG) Program, managed by the National Solar Observatory, which is operated by AURA, Inc., under a cooperative agreement with the National Science Foundation. The data were acquired by instruments operated by the Big Bear Solar Observatory, High Altitude Observatory, Learmonth Solar Observatory, Udaipur Solar Observatory, Instituto de Astrofísica de Canarias, and Cerro Tololo Interamerican Observatory. Electronic Supplementary Material The online version of this article (10.1007/s11207-008-9300-y) contains supplementary material, which is available to authorized users.

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Supplemental Material - 11207_2008_9300_MOESM1_ESM.mov

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Additional details

Created:
August 21, 2023
Modified:
October 19, 2023