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Abstract: The atmosphere of the Sun is characterized by a complex interplay ofcompeting physical processes: convection, radiation, conduction, and magneticfields. The most obvious imprint of the solar convection and its overshootingin the low atmosphere is the granulation pattern. Beside this dominating scalethere is a more or less smooth distribution of spatial scales, both towardssmaller and larger scales, making the Sun essentially a multi-scale object.Convection and overshooting give the photosphere its face but also act asdrivers for the layers above, namely the chromosphere and corona. The magneticfield configuration effectively couples the atmospheric layers on a multitudeof spatial scales, for instance in the form of loops that are anchored in theconvection zone and continue through the atmosphere up into the chromosphereand corona. The magnetic field is also an important structuring agent for thesmall, granulation-size scales, although hydrodynamic shock waves also playan important role - especially in the internetwork atmosphere where mostlyweak fields prevail. Based on recent results from observations and numericalsimulations, we attempt to present a comprehensive picture of the atmosphere ofthe quiet Sun as a highly intermittent and dynamic system.

Autor: S. Wedemeyer-Böhm, A. Lagg, Å. Nordlund


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