Chromospheric structure and dynamics

Details Chromospheric structure and dynamics Chromospheric structure and dynamics

May 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992esasp.344...35s&link_type=abstract

In ESA, Solar Physics and Astrophysics at Interferometric Resolution p 35-42 (SEE N93-10901 01-90)

Physics

1

Chromosphere, Fine Structure, Solar Physics, Spectroscopy, Helioseismology, Line Spectra, Solar Magnetic Field, Solar Oscillations

Scientific paper

Chromospheric structures are observed up to the limiting resolving power of the instruments (less than 0.5 inches). The magnetic field controls the chromospheric topology both at the large scale, such as canopies, supergranulation, mesogranulation and at the small scale, such as fibrils, mottles, and spicules. Different properties of the chromosphere structure may be deduced from a dynamics study. The role of magnetic and convective forces in oscillatory and nonstationary flows observed in the structures is discussed. Spectroscopic diagnostics are used to derive physical parameters in chromospheric structures. Instruments working in spectroscopic mode with a two dimensional field of view are needed. The multichannel double pass spectrographs (Meudon and Pic du Midi in France and Canary Islands) are particularly well adapted to these observations from the ground.

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