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Paper: Chromospheric Diagnostics
Volume: 354, Solar MHD Theory and Observations: A High Spatial Resolution Perspective
Page: 313
Authors: Uitenbroek, H.
Abstract: Several methods for estimating the formation heights of spectral features are explored. For the general non-LTE conditions that prevail in the solar chromosphere the method of response functions seems to be the most appropriate. Examples of the response function for different chromospheric lines in one- and two-dimensional models of the solar atmosphere are shown to illustrate the usefulness of this method. From the shape of the response function for Hα we conclude that current dynamical models are still lacking relevant physics, in particular the influence of magnetic forces, in their upper layers above 500 km.
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