An LTE analysis of the solar photospheric TI I and CR I Spectra - Evidence for non-LTE in excitation

Details An LTE analysis of the solar photospheric TI I and CR I Spectra - Evidence for non-LTE in excitation An LTE analysis of the solar photospheric TI I and CR I Spectra - Evidence for non-LTE in excitation

Jun 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987a%26a...180..229b&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 180, no. 1-2, June 1987, p. 229-240.

Astronomy and Astrophysics

Astrophysics

23

Chromium, Photosphere, Solar Atmosphere, Thermal Analysis, Thermodynamic Equilibrium, Titanium, Line Spectra, Oscillator Strengths, Stellar Models

Scientific paper

An analysis is made of the Ti I(0.0eV-2.3 eV) and CrI (0.94 eV-3.5 eV) lines in the solar photospheric spectrum, using Oxford oscillator strengths and damping constants in conjunction with the Holweger-Mueller solar model atmosphere and a theoretical model constructed following Gustafsson et al. (1975). The 1 eV Ti I lines at disk center give a very narrow minimum dispersion in the (log abundance, microturbulence) diagram with standard deviation 0.014 dex (3.3 percent), but over the whole range of excitation log A changes regularly with multiplet number, reaching a peak at 50 and declining to an apparent constancy at high number In contrast to this, the Cr I lines how a large almost random spread in log A at low excitation, standard deviation 0.098 dex (25 percent), with a tendency to a constant value at high multiplet numbers. It is suggested that these effects are due to non-LTE rather than to errors in the Ti I and Cr I oscillator strengths or the solar equivalent widths. The Cr I lines of multiplet 18 are particularly anomalous. Evidence for a damping enhancement of order 1.1 for 1 eV TiI lines is discussed.

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