Astronomy and Astrophysics – Astrophysics
Scientific paper
Dec 1980
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980ap%26ss..73..379m&link_type=abstract
Astrophysics and Space Science, vol. 73, no. 2, Dec. 1980, p. 379-387.
Astronomy and Astrophysics
Astrophysics
Atmospheric Models, Metallic Stars, Stellar Atmospheres, Stellar Models, Stellar Spectra, Astronomical Models, Hot Stars
Scientific paper
A comparison between model atmosphere grids with and without metal blanketing has been performed in the low-temperature range (Teff equals 6000 K to 10,000 K) and for different metal contents (log A equals 0, -1, -2; A equals scaled solar abundance). For A less than or equal to 0.1 and Teff equal to or greater than 7000 K, the Johnson color indices U - B and B - V, together with the Stromgren u - b, b - y and the bolometric correction are little affected by metal blanketing (Delta mag less than 0.04 m). On the other hand, the trend of the physical quantities and the m1 and c1 color indices reflect the inadequateness of the models even with A equals 0.01 and Teff equals 9500 K, where hydrogen line blanketing is expected to dominate. This fact discourages the use of metal unblanketed atmospheres other than for comparison of color indices or the calculation of bolometric corrections for Population II A-F spectral types.
Moretti Marco
Rossi Luca
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