Titlebook: Energy Storage and Release through the Solar Activity Cycle; Models Meet Radio Ob Christophe Marqué,Alexander Nindos Book 2012 Springer Sci

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https://doi.org/10.1007/978-3-540-71708-9osonic speed, computed from a standard magnetic field model, was estimated as high as ∼ 600 km s., implying that the CME speed was probably just sufficient to drive a weak fast-mode MHD shock ahead of the front. Simultaneously with the type II radio emission, significant changes in the O . doublet l

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Origin of the Submillimeter Radio Emission During the Time-Extended Phase of a Solar Flare,mpulsive phase and can last for a few tens of minutes to more than one hour. The few examples discussed in the literature indicate that such long-lasting submillimeter emission is most likely thermal bremsstrahlung. We present a detailed analysis of the time-extended phase of the 27 October 2003 (M6

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Millisecond Radio Spikes in the Decimetric Band,nts were obtained with a very high time resolution (80 microseconds) radio spectrograph in the 1352 – 1490 MHz range. These data were complemented with observations from the radio spectrograph at Ondřejov in the 0.8 – 2.0 GHz band. We evaluated the basic characteristics of the individual spikes (dur

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Magnetoacoustic Wave Trains in the 11 July 2005 Radio Event with Fiber Bursts,e found structures with different characteristic period . and frequency drift FD: .) fiber substructures (composed of dot emissions) with ..≈ 0.5 s, FD.=− 87 MHz s. on average, .) fiber structures with ..≈1.9 s, and .) drifting structures with ..≈81.4 s, FD.=− 8.7, + 98.5, and − 21.8 MHz s.. In the

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,Quasi-periodic Oscillations of Solar Active Regions in Connection with Their Flare Activity – NoRH level of the chromosphere-corona transition region. The observations of short period (from one to ten minutes) oscillations in sunspots reflect propagation of magnetohydrodynamic (MHD) waves in the magnetic flux tubes of the sunspots. We investigate the oscillation parameters in active regions in c

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