Acoustic wave propagation in the solar atmosphere. IV Nonadiabatic wave excitation with frequency spectra

Details Acoustic wave propagation in the solar atmosphere. IV Nonadiabatic wave excitation with frequency spectra Acoustic wave propagation in the solar atmosphere. IV Nonadiabatic wave excitation with frequency spectra

1997-03-17

arxiv.org/abs/astro-ph/9703106v1

Astronomy and Astrophysics

Astrophysics

12 pages, 11 figures, accepted for publication in A & A

Scientific paper

We study the response of the solar atmosphere to excitations by large amplitude acoustic waves with radiation damping now included. Monochromatic adiabatic waves, due to unbalanced heating, generate continuously rising chromospheric temperature plateaus in which the low frequency resonances quickly die out. All non-adiabatic calculations lead to stable mean chromospheric temperature distributions determined by shock dissipation and radiative cooling. For non-adiabatic monochromatic wave excitation, a critical frequency f_cr ~ 1/25 Hz is confirmed, which separates domains of different resonance behaviour. For waves of frequency f < f_cr, the resonances decay, while for waves of f > f_cr persistent resonance oscillations occur, which are perpetuated by shock merging. Excitation with acoustic frequency spectra produces distinct dynamical mean chromosphere models where the detailed temperature distributions depend on the shape of the assumed spectra. The stochasticity of the spectra and the ongoing shock merging lead to a persistent resonance behaviour of the atmosphere. The acoustic spectra show a distinct shape evolution with height such that at great height a pure 3 min band becomes increasingly dominant. With our Eulerian code we did not find appreciable mass flows at the top boundary.

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