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

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5. Conclusion

We may draw the following conclusions from calculations of the sensitivity indicators presented in this paper:

1. The photospheric lines of Fe I are the most responsive to temperature variations. Even minor temperature fluctuations of the order of 1% can be measured with the help of the most responsive lines. The sensitivity to the temperature is higher than to other atmospheric parameters by approximately 10 times.

2. The sensitivity indicators presented on the plots and in the table may be very valuable for fast and easy analysis of the magnitudes of the response of the line depression to the physical conditions in the solar atmosphere. The estimates of the line sensitivity to pressure and microturbulence are less accurate than to the temperature. The temperature sensitivity indicator table computed for individual lines may be useful for the temperature diagnostics in the photospheric layers, and also for choice of the line with the predominant temperature sensitivity or the group of lines with the same temperature sensitivity. The group of this type is often required for more detailed spectral analysis of the solar and stellar atmospheres.

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© European Southern Observatory (ESO) 1998

Online publication: December 8, 1997
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