Waves in the low solar chromosphere

Details Waves in the low solar chromosphere Waves in the low solar chromosphere

May 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979a%26a....74..273s&link_type=abstract

Astronomy and Astrophysics, vol. 74, no. 3, May 1979, p. 273-279.

Physics

18

Chromosphere, Plasma Waves, Solar Atmosphere, Solar Physics, Data Reduction, Phase Shift, Radial Velocity, Root-Mean-Square Errors, Solar Spectra, Velocity Distribution, Weighting Functions

Scientific paper

Observations of the Mg I line at 5172.7 A made with the Sacramento Peak Solar Tower have been analyzed statistically. The phase shifts between dopplershifts and between intensity and dopplershift fluctuations measured at different points in the Mg I line profile have been interpreted by wave theory, after a discussion of the formation altitudes of dopplershifts. Radiative dissipation seems to be efficient up to an altitude of 600 km, in the evanescent wave range (3-5 mHz). Some energy can be transported, but in the acoustic wave range (5-8 mHz), energy propagation is not detected. The observations in that frequency range are explained by the simultaneous presence of upward propagating waves and waves reflected in the high chromosphere. The presence of pure downward propagating waves around the temperature minimum can be anticipated.

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