Observations of the Solar Chromosphere

Details Observations of the Solar Chromosphere Observations of the Solar Chromosphere

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aspc..354..259j&link_type=abstract

Solar MHD Theory and Observations: A High Spatial Resolution Perspective ASP Conference Series, Vol. 354, Proceedings of the Con

Astronomy and Astrophysics

Astronomy

27

Scientific paper

I summarize observational properties of the solar chromosphere with emphasis on some of Bob Stein's continuing interests, with an historical slant. Bob's interests always concern basic physical processes, so I try to identify some basic facts about the chromosphere from the myriads of observations from radio to UV wavelengths. The observations suggest a simple demarcation between the ``low'' chromosphere and ``high'' chromosphere which depends on the local plasma-β. Relatively simple properties are exhibited in high-β regions (hydrostatic equilibrium, three-minute compressive oscillations), and obviously complex thermal properties of the ``fine structure'' observed for many decades, arise in low-β chromospheric regions. The latter appears to share properties more in common with the intermingled lower corona, where the energetically dominant magnetic structure is arguably simpler than the high-β regions. But like the coronal heating problem, the thermal structure of the upper chromosphere is far more complex and is manifested as fine structure.

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