Other
Scientific paper
Mar 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...405..787f&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 405, no. 2, p. 787-797.
Other
5
Energy Transfer, Magnesium, Photosphere, Solar Atmosphere, Solar Oscillations, Chromosphere, Damping, Plasma Heating, Standing Waves, Thermodynamic Properties, Wave Propagation
Scientific paper
We have measured and analyzed the p-mode oscillations in the profile of the Mg I 4571 A line in a quiet region near disk center. The oscillations are found to be mostly standing waves, in agreement with previous work. However, a small propagating component is measured, and we determine the direction, magnitude, and vertical variation of the energy propagation. The work integral indicates an upward energy flow of about 2 x 10 exp 7 ergs/sq cm/s at a height of 50 km above the base of the photosphere for waves with frequencies of 2-16 mHz. This energy flow decreases exponentially with height and drops below 10 exp 5 ergs/sq cm/s in the uppermost photosphere. The energy flow leaving the upper photosphere is at least an order of magnitude too small to constitute a significant source of heating for the chromosphere. However, the p-mode damping in the lower photosphere approaches levels large enough to account for the measured p-mode line widths. The relative amplitudes and phases of the thermodynamic quantities indicate that the p-mode are neither adiabatic nor isothermal in the photosphere.
Fontenla Juan Manuel
Hathaway David H.
Moore Robert L.
Rabin Doug
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