Response functions and contribution functions of photospheric lines

Astronomy and Astrophysics – Astrophysics

Scientific paper

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Fraunhofer Lines, Line Spectra, Perturbation Theory, Photosphere, Radiative Transfer, Stellar Atmospheres, Electron Density (Concentration), Fraunhofer Line Discriminators, Spectral Energy Distribution, Stellar Spectra, Temperature Distribution, Thermodynamic Equilibrium

Scientific paper

An attempt is made to obtain the response function (RF) of a photospheric Fraunhofer line by solving the equation of radiative transfer in LTE using an appropriate perturbation method. A first-order expression for the RF is derived with which effects of arbitrary perturbations in thermodynamic quantities or velocity-field parameters on emergent line intensity can be evaluated. Perturbations considered to be amenable to such treatment include line-opacity Doppler shifts due to velocity fields, microturbulence variations, and temperature variations at constant electron density. Some examples of RFs for photospheric lines are presented, and an attempt is made to define the contribution function (CF) of a line depression in full analogy with that of the emergent intensity. It is noted that a CF should not be employed in place of the appropriate RF to predict the sensitivity of a Fraunhofer line to a perturbation at a given depth.

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