Simulation of the wave propagation in the 3D solar atmosphere
A theory of wave propagation in the solar atmosphere has been applied to study peculiarities in the wave behaviour above granules and intergranular lanes. We obtained analytical solution of the hydrodynamical equations considering a vertical monochromatic wave propagation in a moving isothermal medium. Effects of the wave reflection were taken into account. We introduced oscillations into a 3D snapshot of the theoretical time dependent solar model atmosphere. NLTE synthesis of the two solar lines was performed: the relatively strong Fe I 5324 Å which is formed over all the photosphere and a weaker Ni I 6768 Å line. The latter is widely used in helioseismology. Both granular and oscillatory components of the velocity field were taken into account. We compared our modeling with the high spatial resolution observations obtained from the ground using VTT on Tenerife and from space using SOHO/MDI. In general, amplitudes and phases of oscillations above granules and intergranular lanes are reproduced by the applied model. We conclude that many differences in oscillations above granules and lanes can be induced by variations of the physical conditions in these structures.
SOHO 10/GONG 2000 Workshop: Helio- and Asteroseismology at the Dawn of the Millennium
- Pub Date:
- January 2001
- SUN: PHOTOSPHERE;