From radiation magnetohydrodynamic (RMHD) simulations of the solar atmosphere we have found a new mechanism for the excitation of longitudinal slow modes within magnetic flux concentrations. It is found that the convective downdrafts in the immediate surroundings of magnetic elements are responsible for the excitation of slow modes. The coupling between the external downdraft and the plasma motion internal to the flux concentration is mediated by the inertial forces of the downdraft that act on the magnetic flux concentration. These forces pump the internal atmosphere in the downward direction, which entails a fast downflow in the photospheric and chromospheric layers of the magnetic element. Subsequent to the transient pumping phase, the atmosphere rebounds, causing a slow mode traveling along the magnetic flux concentration in the upward direction and developing into a shock wave in chromospheric heights, possibly capable of producing some kind of dynamic fibril. This event occurs recurrently. We compare the power spectra of the temperature and velocity of the flux-sheet atmosphere to the corresponding spectra of the unmagnetized atmosphere.
4th Hinode Science Meeting: Unsolved Problems and Recent Insights
- Pub Date:
- May 2012