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Space Science Reviews, 2006
A Brief History of CME Science.- Coronal Mass Ejections: Overview of Observations.- In-Situ Solar Wind and Magnetic Field Signatures of Interplanetary Coronal Mass Ejections.- An Introduction to CMEs and Energetic Particles.- An Introduction to Theory and Models of CMEs, Shocks, and Solar Energetic Particles.- An Introduction to the pre-CME Corona ...
R. von Steiger +4 more
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A Brief History of CME Science.- Coronal Mass Ejections: Overview of Observations.- In-Situ Solar Wind and Magnetic Field Signatures of Interplanetary Coronal Mass Ejections.- An Introduction to CMEs and Energetic Particles.- An Introduction to Theory and Models of CMEs, Shocks, and Solar Energetic Particles.- An Introduction to the pre-CME Corona ...
R. von Steiger +4 more
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Multiple regions of shock-accelerated particles during a solar coronal mass ejection
Nature Astronomy, 2019The Sun is an active star that can launch large eruptions of magnetized plasma into the heliosphere, known as coronal mass ejections (CMEs). These can drive shocks that accelerate particles to high energies, often resulting in radio emission at low ...
D. Morosan +10 more
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Annual Review of Astronomy and Astrophysics, 1984
Sudden expulsions of dense clouds of plasma from the outer atmosphere of the Sun, termed "coronal mass ejections" (CMEs), are the focus of intense observational and theoretical efforts. CMEs are a type of coronal transient, the general name given the disruption of coronal structure.
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Sudden expulsions of dense clouds of plasma from the outer atmosphere of the Sun, termed "coronal mass ejections" (CMEs), are the focus of intense observational and theoretical efforts. CMEs are a type of coronal transient, the general name given the disruption of coronal structure.
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AIP Conference Proceedings, 2000
The most dramatic changes in the solar corona occur during coronal mass ejections, or CMEs, during which solar material is propelled outward into the heliosphere from regions in the corona not previously participating in the solar wind expansion. These ejections often produce major solar wind disturbances, large geomagnetic storms, enhancements of ...
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The most dramatic changes in the solar corona occur during coronal mass ejections, or CMEs, during which solar material is propelled outward into the heliosphere from regions in the corona not previously participating in the solar wind expansion. These ejections often produce major solar wind disturbances, large geomagnetic storms, enhancements of ...
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Geoeffectivity of Coronal Mass Ejections
Space Science Reviews, 2007Coronal mass ejections and post-shock streams driven by them are the most efficient drivers of strong magnetospheric activity, magnetic storms. For this reason there is considerable interest in trying to make reliable forecasts for the effects of CMEs as much in advance as possible. To succeed this requires understanding of all aspects related to CMEs,
K. E. J. Huttunen +3 more
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Coronal Mass Ejections: Overview of Observations
Space Science Reviews, 2006We survey the subject of Coronal Mass Ejections (CMEs), emphasizing knowledge available prior to about 2003, as a synopsis of the phenomenology and its interpretation.
Hudson, H. S. +2 more
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Reviews of Geophysics, 1987
While the first coronal mass ejections (CMEs) were observed with the OSO‐7 white light coronagraph (Tousey, 1973), it was the Skylab coronagraph observations that clearly established CMEs as an important component of solar coronal physics. CMEs have been defined by Hundhausen et al.
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While the first coronal mass ejections (CMEs) were observed with the OSO‐7 white light coronagraph (Tousey, 1973), it was the Skylab coronagraph observations that clearly established CMEs as an important component of solar coronal physics. CMEs have been defined by Hundhausen et al.
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Radio Signatures of Coronal Mass Ejection Interaction: Coronal Mass Ejection Cannibalism?
The Astrophysical Journal, 2001We report the first detection at long radio wavelengths of interaction between coronal mass ejections (CMEs) in the interplanetary medium. The radio signature is in the form of intense continuum-like radio emission following an interplanetary type II burst. At the time of the radio enhancement, coronagraphic images show a fast CME overtaking a slow CME.
J. L. Bougeret +4 more
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1999
Coronal mass ejections are seen as bright features that move outward through the solar corona at speeds from 10 to about 2,000 km s-1. They involve the expulsion of substantial quantities of plasma from large regions of the corona. The spectacular nature of the largest mass ejections is illustrated in Figure 5.1 by a time sequence of four images ...
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Coronal mass ejections are seen as bright features that move outward through the solar corona at speeds from 10 to about 2,000 km s-1. They involve the expulsion of substantial quantities of plasma from large regions of the corona. The spectacular nature of the largest mass ejections is illustrated in Figure 5.1 by a time sequence of four images ...
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Coronal mass ejections: structure and dynamics
Plasma Physics and Controlled Fusion, 2009We discuss in this paper some issues related to the relationship, currently thought to be relatively strong, between large scale solar eruptive events and twisted magnetic flux ropes (TFRs). We first consider the possibility to prove the presence of a TFR in a pre-eruptive configuration by using a model along with observational information provided by ...
J J Aly, Tahar Amari, Tahar Amari
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