Physical structure of solar cool loops.
Abstract
Recently, studies and observations focused on the solar transition region and the low corona have shown the importance of small and cool magnetic loops in producing most of the solar EUV output at temperatures below 1 MK. This kind of structures has remained only poorly characterized in terms of physical properties. We study the possibility of obtaining cool loops using unidimensional hydrodynamic simulations, performed with a state-of-the-art numerical code with a fully adaptive grid. The dependence of their physical structures on the form of the radiative losses function has been explored. We find, as a first result, that the shape of the radiative losses function for T<105 K imposes restrictive conditions on the existence and the stability of such cool loops.
- Publication:
-
Memorie della Societa Astronomica Italiana Supplementi
- Pub Date:
- 2012
- Bibcode:
- 2012MSAIS..19...81S
- Keywords:
-
- Hydrodynamics;
- Sun: corona;
- Sun: transition region