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We present results of non-LTE modeling of H-alpha 6563 A and Mg II k&h 2796 Aand 2803 A lines. This modeling is important for interpretation of coordinatedobservations from the recently launched NASA's IRIS mission and from the NewSolar Telescope at Big Bear Solar Observatory. Among available codes for thenon-LTE modeling, the RH code is chosen as the most appropriate for modeling ofthe line profiles. The most suitable Hydrogen and Magnesium atomic models areselected by performing several tests of the code. The influence of theionization degree on the line profiles is also studied. Radiative-MHDsimulations of the solar atmosphere, obtained with the Bifrost code, are usedas input data for calculation of synthetic spectra of the H-alpha and Mg II h&klines for particular locations evolving with time. The spectral line variationsreveal the presence of MHD waves in the simulation results. We constructoscillation power spectra of the line intensity for different wavelength, andcompare these with the corresponding height-dependent power spectra ofatmospheric parameters from the simulations. We find correlations between thepower spectra of intensities of the line profiles at certain wavelengths andthe power spectra of the atmospheric parameters at the tau-unity heights forthese wavelengths. These results provide a new diagnostic method ofchromospheric oscillations; however, larger amounts of data are needed toconfirm these correlations.

Using MHD simulations to model H-alpha and UV spectral lines for interpretation of IRIS and NST data