Statistics – Computation
Scientific paper
Jul 1987
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987mnras.227..135l&link_type=abstract
Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 227, July 1, 1987, p. 135-141. Research supported by Er
Statistics
Computation
11
A Stars, Computational Astrophysics, Radiant Flux Density, Spectral Energy Distribution, Stellar Color, Ion Production Rates, M Stars, Metallicity, Stellar Temperature
Scientific paper
The Am stars are observed to have excess flux at λ-1 = 2.09 μm-1 (λ = 4785 Å) compared with the predicted fluxes of line blanketed model stellar atmospheres or with the fluxes of normal stars. This excess flux affects both the Strömgren b-magnitude and the β index so that the effective temperature of an Am star derived from these measures is erroneously high. The use of the contaminated b-magnitude in the construction of the c1 and m1 indices leads to surface gravities and metallicities that are too large. The best way to avoid these hazards is to use the full energy distribution. Synthetic spectra of the blue spectral region show that the excess flux is not due to elements, such as calcium and scandium, that are deficient in Am stars. It is suggested that the enhanced brightness near 2.09 μm-1 might be due to a change in the ionization balance of the iron-peak elements.
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