Interpretation of emission line profiles of rotating shells

Details Interpretation of emission line profiles of rotating shells Interpretation of emission line profiles of rotating shells

Apr 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981a%26a....97..175p&link_type=abstract

Astronomy and Astrophysics, vol. 97, no. 1, Apr. 1981, p. 175-181.

Astronomy and Astrophysics

Astrophysics

8

B Stars, Emission Spectra, Line Spectra, Stellar Rotation, Stellar Spectra, Rotating Bodies, Shells (Structural Forms), Spherical Shells, Stellar Atmospheres

Scientific paper

Simple model calculations are carried out in order to demonstrate how shell properties (geometry, density gradient and rotation) influence the emission line profile. A convenient method is given which allows to derive shell parameters from measured line profiles. The procedure is applied to the Be stars EW Lac, HD 193182, Pi Aqr, Beta Mon, 66 Oph, Kappa Dra, Zeta Tau, Psi Per, Phi Per. The resulting rotational velocities are comparable with those derived from photospheric lines. That means that the emitting region of all the stars considered begins at the stellar photosphere. The radial extensions of these regions are between 3 and 5 photospheric radii. The density gradient does not show a severe deviation from that produced by continuous mass flow.

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