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The Solar Origin of Corotating Interaction Regions and Their Formation in the Inner Heliosphere |
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| Authors: | A Balogh V Bothmer NU Crooker RJ Forsyth G Gloeckler A Hewish M Hilchenbach R Kallenbach B Klecker JA Linker E Lucek G Mann E Marsch A Posner IG Richardson JM Schmidt M Scholer Y-M Wang RF Wimmer-Schweingruber MR Aellig P Bochsler S Hefti Z Mikić |
| Institution: | 1. The Blackett Laboratory, Imperial College, London, United Kingdom 2. Extraterrestrische Physik, Universit?t Kiel, Kiel, Germany 3. Center for Space Physics, Boston University, Boston, Massachussetts, USA 4. Dept. of Physics and IPST, University of Maryland, College Park, Maryland, USA 5. Dept. of Atmosph., Oceanic, and Space Sciences, University of Michigan, Ann Arbor, Mich., USA 6. Mullard Radio Astronomy Observatory, Cavendish Laboratory, Cambridge, United Kingdom 7. Max-Planck-Institut für Aeronomie, Katlenburg-Lindau, Germany 8. International Space Science Institute, Bern, Switzerland 9. Max-Planck-Institut für Extraterrestrische Physik, Garching, Germany 10. Science Applications International Corporation, San Diego, California, USA 11. Astrophysikalisches Institut, Potsdam, Germany 12. NASA/Goddard Space Flight Center, Greenbelt, Maryland, USA 13. E.O. Hulburt Center for Space Research, Naval Research Laboratory, Washington, DC, USA 14. Physikalisches Institut der Universit?t Bern, Bern, Switzerland |
| Abstract: | Corotating Interaction Regions (CIRs) form as a consequence of the compression of the solar wind at the interface between fast speed streams and slow streams. Dynamic interaction of solar wind streams is a general feature of the heliospheric medium; when the sources of the solar wind streams are relatively stable, the interaction regions form a pattern which corotates with the Sun. The regions of origin of the high speed solar wind streams have been clearly identified as the coronal holes with their open magnetic field structures. The origin of the slow speed solar wind is less clear; slow streams may well originate from a range of coronal configurations adjacent to, or above magnetically closed structures. This article addresses the coronal origin of the stable pattern of solar wind streams which leads to the formation of CIRs. In particular, coronal models based on photospheric measurements are reviewed; we also examine the observations of kinematic and compositional solar wind features at 1 AU, their appearance in the stream interfaces (SIs) of CIRs, and their relationship to the structure of the solar surface and the inner corona; finally we summarise the Helios observations in the inner heliosphere of CIRs and their precursors to give a link between the optical observations on their solar origin and the in-situ plasma observations at 1 AU after their formation. The most important question that remains to be answered concerning the solar origin of CIRs is related to the origin and morphology of the slow solar wind. This revised version was published online in August 2006 with corrections to the Cover Date. |
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