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• W2128482204 abstract "Coronal mass ejections (CMEs) have been recognized as the most energetic phenomenon in the heliosphere, deriving their energy from the stressed magnetic fields on the Sun. This paper highlights some of the recent results on CMEs obtained from the Solar and Heliospheric Observatory (SOHO) and the Solar Terrestrial Relations Observatory (STEREO) missions. The summary of the talk follows. SOHO observations revealed that the CME rate is almost a factor of two larger than previously thought and varied with the solar activity cycle in a complex way (e.g., high-latitude CMEs occurred in great abundance during the solar maximum years). CMEs were found to interact with other CMEs as well as with other large-scale structures (coronal holes), resulting in deflections and additional particle acceleration. STEREO observations have confirmed the three-dimensional nature of CMEs and the shocks surrounding them. The EUV signatures (flare arcades, corona) dimming, filament eruption, and EUV waves) associated with CMEs have become vital in the identification of solar sources from which CMEs erupt. CMEs with speeds exceeding the characteristic speeds of the corona and the interplanetary medium drive shocks, which produce type II radio bursts. The wavelength range of type II bursts depends on the CME kinetic energy: type II bursts with emission components at all wavelengths (metric to kilometric) are due to CMEs of the highest kinetic energy. Some CMEs, as fast as 1600 km/s do not produce type II bursts, while slow CMEs (400 km/s) occasionally produce type II bursts. These observations can be explained as the variation in the ambient flow speed (solar wind) and the Alfven speed. Not all CME-driven shocks produce type II bursts because either they are subcritical or do not have the appropriate geometry. The same shocks that produce type II bursts also produce solar energetic particles (SEPs), whose release near the Sun seems to be delayed with respect to the onset of type II bursts. This may indicate a subtle difference in the acceleration of the ions and 10 keV electrons needed to produce type II bursts. Surprisingly, some shocks lacking type II bursts are associated with energetic storm particle events (ESPs) pointing to the importance of electron escape from the shock for producing the radio emission. CMEs slow down or accelerate in the interplanetary medium because of the drag force, which modifies the transit time of CMEs and shocks. Halo CMEs that appear to surround the occulting disk were known before the SOHO era as occasional events. During the SOHO era, they became very prominent because of their ability to impact Earth and producing geomagnetic storms. Halo CMEs are generally more energetic than ordinary CMEs, which means they can produce severe impact on Earth's magnetosphere. Their origin close to the disk center of the Sun ensures direct impact on the magnetosphere, although their internal magnetic structure is crucial in causing storms. The solar sources of CMEs that produce SEP events at Earth, on the other hand, are generally in the western hemisphere because of the magnetic connectivity. Thus, CMEs are very interesting from the point of view of plasma physics as well as practical implications because of their space weather impact." @default.
• W2128482204 created "2016-06-24" @default.
• W2128482204 creator A5015019188 @default.
• W2128482204 creator A5047585293 @default.
• W2128482204 date "2010-05-31" @default.
• W2128482204 modified "2023-09-25" @default.
• W2128482204 title "Coronal Mass Ejections: a Summary of Recent Results" @default.
• W2128482204 cites W105604055 @default.
• W2128482204 cites W110002938 @default.
• W2128482204 cites W1492579793 @default.
• W2128482204 cites W1495313431 @default.
• W2128482204 cites W1511195911 @default.
• W2128482204 cites W1549349995 @default.
• W2128482204 cites W1554908506 @default.
• W2128482204 cites W1579924745 @default.
• W2128482204 cites W1608215932 @default.
• W2128482204 cites W1610587877 @default.
• W2128482204 cites W1613816320 @default.
• W2128482204 cites W1630984028 @default.
• W2128482204 cites W1663178787 @default.
• W2128482204 cites W1666384313 @default.
• W2128482204 cites W1667149317 @default.
• W2128482204 cites W1873216632 @default.
• W2128482204 cites W1967594029 @default.
• W2128482204 cites W1968056726 @default.
• W2128482204 cites W1968256717 @default.
• W2128482204 cites W1972994815 @default.
• W2128482204 cites W1974776769 @default.
• W2128482204 cites W1978888974 @default.
• W2128482204 cites W1980425192 @default.
• W2128482204 cites W1981878130 @default.
• W2128482204 cites W1982239057 @default.
• W2128482204 cites W1985214372 @default.
• W2128482204 cites W1988775960 @default.
• W2128482204 cites W1989453610 @default.
• W2128482204 cites W1996900815 @default.
• W2128482204 cites W1998110593 @default.
• W2128482204 cites W1999049503 @default.
• W2128482204 cites W2001591270 @default.
• W2128482204 cites W2005650738 @default.
• W2128482204 cites W2008856055 @default.
• W2128482204 cites W2010184544 @default.
• W2128482204 cites W2012429686 @default.
• W2128482204 cites W2012461664 @default.
• W2128482204 cites W2012608316 @default.
• W2128482204 cites W2019210943 @default.
• W2128482204 cites W2019732516 @default.
• W2128482204 cites W2021807045 @default.
• W2128482204 cites W2022940101 @default.
• W2128482204 cites W2023855736 @default.
• W2128482204 cites W2031795489 @default.
• W2128482204 cites W2036167857 @default.
• W2128482204 cites W2036617303 @default.
• W2128482204 cites W2037397531 @default.
• W2128482204 cites W2041572965 @default.
• W2128482204 cites W2041779504 @default.
• W2128482204 cites W2042641148 @default.
• W2128482204 cites W2043780303 @default.
• W2128482204 cites W2048346284 @default.
• W2128482204 cites W2050344634 @default.
• W2128482204 cites W2053092803 @default.
• W2128482204 cites W2054863294 @default.
• W2128482204 cites W2055984471 @default.
• W2128482204 cites W2056890589 @default.
• W2128482204 cites W2057313607 @default.
• W2128482204 cites W2066527046 @default.
• W2128482204 cites W2066662599 @default.
• W2128482204 cites W2069262502 @default.
• W2128482204 cites W2073171677 @default.
• W2128482204 cites W2073671951 @default.
• W2128482204 cites W2078281895 @default.
• W2128482204 cites W2081560761 @default.
• W2128482204 cites W2082231290 @default.
• W2128482204 cites W2086458577 @default.
• W2128482204 cites W2087539926 @default.
• W2128482204 cites W2088193747 @default.
• W2128482204 cites W2092523780 @default.
• W2128482204 cites W2094912575 @default.
• W2128482204 cites W2098901213 @default.
• W2128482204 cites W2102300459 @default.
• W2128482204 cites W2104248815 @default.
• W2128482204 cites W2108179399 @default.
• W2128482204 cites W2119209514 @default.
• W2128482204 cites W2124951042 @default.
• W2128482204 cites W2133645651 @default.
• W2128482204 cites W2147222167 @default.
• W2128482204 cites W2148977061 @default.
• W2128482204 cites W2156722592 @default.
• W2128482204 cites W2162254832 @default.
• W2128482204 cites W2170491912 @default.
• W2128482204 cites W2571403449 @default.
• W2128482204 cites W2983717917 @default.
• W2128482204 cites W3007332436 @default.
• W2128482204 cites W3014690241 @default.
• W2128482204 cites W3016532862 @default.
• W2128482204 cites W3099552328 @default.
• W2128482204 cites W3107418010 @default.
• W2128482204 cites W3110924573 @default.
• W2128482204 cites W45822971 @default.
• W2128482204 cites W86172238 @default.

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