Characterizing Chromospheric Condensation from Shocks Driven by Thermal Conduction
Abstract
Chromospheric condensation is a downflow accompanied by a hydrodynamic shock which accompanies the energy release by magnetic reconnection in a solar flare. While this component of a flare reflects the energy release process only indirectly, it can be observed at the highest spatial and temporal resolution, even from the ground. It is therefore important to establish a quantitative relationship between energy release and condensation properties. In this initial investigation we consider only energy transport via thermal conduction. We develop an analytical solution to the decay of the condensation under the influence of gravitational density stratification. This provides a relationship between shock velocity and pre-shock density. We also use one-dimensional gas-dynamic numerical simulations to explore the dynamics of these shocks as they penetrate into the stratified chromosphere. These suggest that the shock decay can be de-composed into two different phases, whose properties vary with gravitational scale height and the flare energy flux.
- Publication:
-
AGU Fall Meeting Abstracts
- Pub Date:
- December 2020
- Bibcode:
- 2020AGUFMSH057..07A
- Keywords:
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- 7507 Chromosphere;
- SOLAR PHYSICS;
- ASTROPHYSICS;
- AND ASTRONOMY;
- 7509 Corona;
- SOLAR PHYSICS;
- ASTROPHYSICS;
- AND ASTRONOMY;
- 7519 Flares;
- SOLAR PHYSICS;
- ASTROPHYSICS;
- AND ASTRONOMY;
- 7526 Magnetic reconnection;
- SOLAR PHYSICS;
- ASTROPHYSICS;
- AND ASTRONOMY