The Evolution of Some Physical Parameters in the DACs/SACs Regions in Be Stellar Atmospheres

Details The Evolution of Some Physical Parameters in the DACs/SACs Regions in Be Stellar Atmospheres The Evolution of Some Physical Parameters in the DACs/SACs Regions in Be Stellar Atmospheres

Sep 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aipc..938..176l&link_type=abstract

SPECTRAL LINE SHAPES IN ASTROPHYSICS: VI Serbian Conference on Spectral Line Shapes in Astrophysics (VI SCSLSA). AIP Conference

Astronomy and Astrophysics

Astrophysics

1

Stellar Atmospheres, Radiative Transfer, Opacity And Line Formation, Atomic And Molecular Data, Spectra, And Spectral Parameters, Emission-Line Stars, Circumstellar Shells, Clouds, And Expanding Envelopes, Circumstellar Masers

Scientific paper

In order to analyse the stellar spectra we use the Gauss-Rotation method and we conclude that the SACs/DACs phenomena are able to explain, in a unique way, the complex and peculiar observed profiles. These results arise from the study of the Mg II (λλ 2795.523, 2802.698 Å), SiIV (λλ 1393.755, 1402.77 Å), and Hα (λ 6562,817 Å) region of a great number of Be stars of all spectral subtypes and luminosity classes (64 in the case of Mg II resonance lines and 70 in the case of Si IV resonance limes). For the study of the regions which create the complex Hα line profiles we analyzed the OHP (Observatory of Haute Provence) spectrographs of 120 Be stars of all spectral subtypes and luminosity classes. We present the evolution of some kinematical parameters from the photosphere to the extreme cool envelope.

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