Radiative equilibrium in solar prominences reconsidered
1 Astronomical Institute, Academy of Sciences of the Czech Republic, 25165 Ondřejov, Czech Republic
2 Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, 85740 Garching, Germany
Received: 23 October 2009
Accepted: 17 December 2011
Aims. We reconsider the question which kinetic temperatures can lead to prominence configurations that are in radiative equilibrium. We compare these temperatures to those from other calculations.
Methods. For this purpose we solved the full non-LTE radiative-transfer problem for a gas consisting of hydrogen, helium and calcium. We used simple isobaric 1D slabs and began with isothermal models. Then we solved the radiative-relaxation problem and determined the radiative-equilibrium conditions within the whole slab.
Results. By adding the calcium radiative losses, we found that these equilibrium temperatures are considerably lower than those obtained for a pure hydrogen gas. This is because the newly calculated CaII line losses appear to play a significant role in the energy balance, similar to chromospheric conditions. The equilibrium temperatures obtained span the range between 4400−9500 K, depending on the gas pressure and slab thickness.
Key words: radiative transfer / Sun: filaments, prominences / line: formation
© ESO, 2012