Radiative transfer in fine structures of solar prominences

In the first part we used Ambartsumains method of addition of layers to show that various problems of radiative transfer in a plane-parallel inhomogeneous atmosphere may be reduced to the solution of the cauchy problems for linear differential equations. The idea of the approach is that we start with the determining of the reflection and transmission coefficients of an atmosphere by solving the initial-value problem for a set of linear differential equations of the first order. After that the internal radiation field is found immediately without solving any new equation.There are some solar prominence fine structures which are not observable. Thus, we need to use theoretical methods to study their geometric and physical properties. It is believed that observed intensities and their fluctuations are related to such fine structures in the line of sight. Regarding the fact that the spectrum line corresponding to the transition will not be sharp and will have a spread in frequency that can be described by absorption profiles. So, the second part of the present study is an attempt to determine the intensity fluctuations in the frequency-dependent case with different absorption profiles such as Doppler, Voigt and Lorentz profiles. It became evident that the intensity fluctuations vary with absorption profile and optical depth variations in the line of sight. It should be noted that the present study focuses on the LTE absorbing atmosphere.