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Multi-Wavelength Observations of CMEs and Associated Phenomena |
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| Authors: | M Pick T G Forbes G Mann H V Cane J Chen A Ciaravella H Cremades R A Howard H S Hudson A Klassen K L Klein M A Lee J A Linker D Maia Z Mikic J C Raymond M J Reiner G M Simnett N Srivastava D Tripathi R Vainio A Vourlidas J Zhang T H Zurbuchen N R Sheeley C Marqué |
| Institution: | 1. LESIA, UMR, 8109 CNRS, Observatoire de Paris, Meudon, France 2. Institute for the Study of Earth, Oceans, and Space, Univ. of New Hampshire, Durham, NH, USA 3. Astrophysikalisches Institut Potsdam, Potsdam, Germany 4. Laboratory for High Energy Astrophysics, NASA/GSFC, Greenbelt, MD, USA 5. Bruny Island Radio Spectrometer, Tasmania, Australia 6. Plasma Physics Division, US Naval Research Laboratory, Washington, DC, USA 7. INAF Osservatorio Astronomico di Palermo, Palermo, Italy 8. Max-Planck-Institut für Sonnenforschung, Katlenburg-Lindau, Germany 9. E. O. Hulburt Center for Space Research, Naval Research Laboratory, Washington, DC, USA 10. Space Sciences Laboratory, University of California, Berkeley, CA, USA 11. Science Applications International Corporation, San Diego, CA, USA 12. CICGE, Observatório Astronómico Prof. Manuel de Barros, Faculdade de Ciências da Universidade do Porto, Vila Nova de Gaia, Portugal 14. Center for Solar Physics and Space Weather, Catholic University of America, Washington, DC, USA 15. NASA, Goddard Space Flight Center, Greenbelt, MD, USA 16. School of Physics and Space Research, University of Birmingham, Birmingham, U.K. 17. Udaipur Solar Observatory, Physical Research Laboratory, Udaipur, India 18. Department of Physical Sciences, University of Helsinki, Helsinki, Finland 19. Center for Earth Observing and Space Research, Institute for Computational Sciences, George Mason University, Fairfax, VA, USA 20. Dept. of Atmospheric, Oceanic, and Space Sciences, Univ. of Michigan, Ann Arbor, MI, USA |
| Abstract: | This chapter reviews how our knowledge of CMEs and CME-associated phenomena has been improved, since the launch of the SOHO mission, thanks to multi-wavelength analysis. The combination of data obtained from space-based experiments and ground based instruments allows us to follow the space-time development of an event from the bottom of the corona to large distances in the interplanetary medium. Since CMEs originate in the low solar corona, understanding the physical processes that generate them is strongly dependant on coordinated multi-wavelength observations. CMEs display a large diversity in morphology and kinematic properties, but there is presently no statistical evidence that those properties may serve to group them into different classes. When a CME takes place, the coronal magnetic field undergoes restructuring. Much of the current research is focused on understanding how the corona sustains the stresses that allow the magnetic energy to build up and how, later on, this magnetic energy is released during eruptive flares and CMEs. Multi-wavelength observations have confirmed that reconnection plays a key role during the development of CMEs. Frequently, CMEs display a rather simple shape, exhibiting a well known three-part structure (bright leading edge, dark cavity and bright knot). These types of events have led to the proposal of the ‘`standard model’' of the development of a CME, a model which predicts the formation of current sheets. A few recent coronal observations provide some evidence for such sheets. Other more complex events correspond to multiple eruptions taking place on a time scale much shorter than the cadence of coronagraph instruments. They are often associated with large-scale dimming and coronal waves. The exact nature of these waves and the physical link between these different manifestations are not yet elucidated. We also discuss what kind of shocks are produced during a flare or a CME. Several questions remain unanswered. What is the nature of the shocks in the corona (blast-wave or piston-driven?) How they are related to Moreton waves seen in Hα? How they are related to interplanetary shocks? The last section discusses the origin of energetic electrons detected in the corona and in the interplanetary medium. “Complex type III-like events,”which are detected at hectometric wavelengths, high in the corona, and are associated with CMEs, appear to originate from electrons that have been accelerated lower in the corona and not at the bow shock of CMEs. Similarly, impulsive energetic electrons observed in the interplanetary medium are not the exclusive result of electron acceleration at the bow shocks of CMEs; rather they have a coronal origin. |
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