Abstract
We expect a variety of dynamic phenomena in the ‘quiescent’ non-flaring corona. Plasma flows, such as siphon flows or convective flows of chromospheric material evaporating into the corona, are expected whenever a pressure differences is established either between the footpoints or between the coronal and chromospheric segments of a coronal loop. Such flows can induce phenomena of spatial and temporal brightness variability of the corona. In particular, evaporation induces a net mass input into the corona and consequently coronal density enhancements. Flows are also expected in the regions where energy is released during magnetic reconnection. From the observational point of view the dynamics of the solar atmosphere has been investigated in great detail mostly in the lower transition region with the HRTS, and during flares with the Solar Maximum Mission and Yohkoh. The high spectral, temporal and spatial resolution of the SOHO ultraviolet spectrometers should enable us in the near future to fill the gap providing a continuous coverage from the chromosphere to the corona, in the 104 -106 K domain, and therefore to best study the dynamics throughout the solar atmosphere.
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Antonucci, E. (1994). Soho Contribution to the Understanding of Mass Supply and Flows in the Solar Corona. In: Fleck, B., Noci, G., Poletto, G. (eds) Mass Supply and Flows in the Solar Corona. Springer, Dordrecht. https://doi.org/10.1007/978-94-011-0930-7_26
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DOI: https://doi.org/10.1007/978-94-011-0930-7_26
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