Computation of model atmospheres and spectra of hot stars by programme SMART: results and problems

Details Computation of model atmospheres and spectra of hot stars by programme SMART: results and problems Computation of model atmospheres and spectra of hot stars by programme SMART: results and problems

Oct 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007smma.conf..236s&link_type=abstract

Spectroscopic methods in modern astrophysics. Proceedings of the conference held 13-15 September 2006, Moscow, Russia. Eds. L. M

Astronomy and Astrophysics

Astrophysics

1

Scientific paper

Program SMART has been composed for computation of model atmospheres of hot stars of arbitrary chemical composition and their synthetic spectra, and also for study of different physical processes in stellar atmospheres. Main advantages of SMART are shortness, simplicity, user friendliness and flexibility for study of different physical processes. Lack of subroutines for computing convection and molecular absorption in the present version of SMART means that it is applicable only to effective temperatures exceeding 9000 K. A new pan-spectral method for determination of chemical composition of stellar atmospheres has been proposed. The method is based on a weighted cumulative width of spectral lines for an element or ion studied. We applied this method to find abundances of 12 elements in the atmosphere of chemically peculiar star HD 175640 observed by Castelli and Hubrig (2004). Our results are in good agreement with the results by Castelli and Hubrig, who analyzed observations using software by Kurucz (1993, 1997).

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