Astronomy and Astrophysics – Astrophysics
Scientific paper
May 1987
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987a%26a...177..292u&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 177, no. 1-2, May 1987, p. 292-302.
Astronomy and Astrophysics
Astrophysics
33
Acoustic Propagation, Line Spectra, Magnetic Flux, Solar Atmosphere, Solar Spectra, Chromosphere, Emission Spectra, K Lines, Mass Flow, Shock Wave Propagation
Scientific paper
The propagation of acoustic waves through vertical magnetic flux tubes in the solar atmosphere was computed with radiation damping by (non-LTE) emission from H(-) and the Mg II k line. Waves of various amplitudes and periods were investigated in flux tubes with three different spreading rates characterized by the radius as a: (1) constant, (2) linear or (3) exponential function of height. The geometry of the flux tubes greatly influences the behavior of the waves. Large wave amplitudes and intense postshock radiative relaxation zones are found in constant tubes while small amplitudes and weak radiation zones were found in exponential tubes. In all calculations following Mg II ionization, transition-layer-like rapid temperature rises formed and transient mass flows were initiated. In constant tubes the rapid temperature rises occurred at low heights while in exponential tubes these layers were found much higher. Waves with longer periods produced steep temperature rises at lower height and led to more mass motion. The heights of the rapid temperature rises did not depend much on the initial wave energy flux.
Kalkofen Wolfgang
Muchmore D.
Ulmschneider Peter
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