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Astron. Astrophys. 329, 721-724 (1998)

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1. Introduction

Often, the diagnostics of stellar atmospheres requires lines more sensitive to one atmospheric parameter and less sensitive to others. To execute a correct choice of such lines, we offer to apply sensitivity indicators. The calculation of sensitivity indicators is based on the use of the depression response functions [FORMULA] (Magain 1986). The detailed description of the calculation techniques was already announced in Sheminova (1993, 1995). The response function defines the rate of variation in the line depression [FORMULA] at every point x in the atmosphere relative to the rate of variation of the atmospheric parameter [FORMULA], which undergoes the local disturbance [FORMULA]. If we integrate the response function [FORMULA] with respect to x and divide it by the value of the emerging depression [FORMULA], we obtain a dimensionless quantity [FORMULA], which is a variation in the observed line depression, [FORMULA], relative to the local variation [FORMULA]:

[EQUATION]

We call it the sensitivity indicator of the line depression.

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© European Southern Observatory (ESO) 1998

Online publication: December 8, 1997
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