Chromosphere and Transition Zone Dynamics and Heating: Need for Future Space Missions

Details Chromosphere and Transition Zone Dynamics and Heating: Need for Future Space Missions Chromosphere and Transition Zone Dynamics and Heating: Need for Future Space Missions

Nov 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006ihy..worke..34d&link_type=abstract

2nd UN/NASA Workshop on International Heliophysical Year and Basic Space Science. Proceedings of the conference held 27 Novembe

Astronomy and Astrophysics

Astrophysics

Scientific paper

SOHO and TRACE observations have clearly shown that even the very quietest part of the solar chromosphere is very structured and dynamic with brightenings and waves. Diagnostics from this region are very difficult because spectral lines are neither formed in LTE nor under optically thin conditions that prevail higher in the Transition Zone. The gas goes from being dominated by the gas pressure in the photosphere to being dominated by the magnetic pressure in the upper chromosphere, involving steep gradients to obtain significant dissipation or heating. The ionization balance of important elements is furthermore out of equilibrium. A proper understanding thus demands very high spatial resolution with accurate measurements of velocity and line width, uninterrupted in Space, across a broad range of temperature ("heights"), to distinguish between wave heating and reconnection events in the chromosphere and Transition Zone. Complex modeling, that ideally should include non-LTE radiative transfer in 3D including the dynamic driving in the convection zone, non- equilibrium ionization, magnetic fields, the transition region and the corona, will be necessary to understand these observations. We will discuss various aspects of this very complex problem and insist on ground measures and, above all, Future Space Missions which should better address Doppler information, temperature coverage and discrimination and, most important, very high spatial resolution to progress on the way to a fully comprehensive view of chromospheric and coronal heating.

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