Volume 378, Number 3, November II 2001
|Page(s)||861 - 882|
|Section||Interstellar and circumstellar matter|
|Published online||15 November 2001|
An atlas of Hγ, He I 4471 and Mg II 4481 lines
DASGAL, UMR 8633 du CNRS, Observatoire de Paris-Meudon, 92195 Meudon, France
2 Institut d'Astrophysique de Paris, CNRS, 98bis Bld. Arago, 75014 Paris, France
3 Facultad de Ciencias Astronómicas y Geofísicas, Universidad de La Plata, Paseo del Bosque S/N, 1900 La Plata, Argentina
Corresponding author: J. Zorec, firstname.lastname@example.org
Accepted: 16 August 2001
We present an atlas of Hγ, He i λ 4471 and Mg ii λ 4481 line profiles obtained in a 10 year observation period of 116 Be stars, which enabled many of them to be observed at quite different emission epochs. From the best fit of the observed He i λ 4471 line profiles with non-LTE, uniform () and full limb-darkened model line profiles, we determined the of the program stars. To account, to some degree, for the line formation peculiarities related to the rapid rotation-induced non-uniform distributions of temperature and gravity on the stellar surface, the fit was achieved by considering () as free parameters. This method produced estimations that correlate with the rotational velocities determined by Slettebak (1982) within a dispersion 30 km s-1 and without any systematic deviation. They can be considered as given in the new Slettebak's et al. (1975) system. Only 13 program stars have discrepant values. In some objects, this discrepancy could be attributed to binary effects. Using the newly determined parameters, we found that the ratio of true rotational velocities of the program Be stars has a very low dispersion around the mean value. Assuming then that all the stars are rigid rotators with the same ratio , we looked for the value of that better represents the distribution of for randomly oriented rotational axes. We obtained . This value enabled us to determine the probable inclination angle of the stellar rotation axis of the program stars. In the observed line profiles of Hγ, He i λ 4471, Mg ii λ 4481 and Fe ii λ 4351 we measured several parameters related to the absorption and/or emission components, such as: equivalent width, residual emission and/or absorption intensity, FWHM, emission peak separations, etc. The parameters related to the Hγ line emission profiles were used to investigate the structure of the nearby environment of the central star. From the characteristics of the correlations between these quantities and the inferred inclination angle, we concluded that in most of cases the Hγ line emission forming regions may not be strongly flattened. Using a simple representation of the radiation flux emitted by the star+envelope system, we derived first order estimates of physical parameters characterizing the Hγ line emission formation region. Thus, we obtained that the total extent of the Hγ region is and that the density distribution in these layers can be mimicked with a power law , where . The same approach enabled us to estimate the optical depth of the Hγ line emission formation region. From its dependence with the aspect angle, we concluded that these regions are caracterized by a modest flattening and that the density contrast of the circumstellar envelope near the star should be two orders of magnitude lower than predicted by models based on a priori disc-shaped circumstellar envelopes. We found that the separation between the emission peaks, , and the full width at half maximum, , of the Hγ line emission are not only sensitive to kinematic effects, but to line optical depth as well. This finding agrees with previous theoretical predictions and confirms that Huang's (1972) relation overestimates the extent of the Hγ line emission formation region.
Key words: stars: emission-line, Be / stars: fundamental parameters / techniques: spectroscopic / line: profiles
Data obtained at CASLEO operated under agreement between the CONICET and the National Universities of La Plata, Córdoba and San Juan, Argentina, at ESO La Silla, Chile and at OHP, France.
© ESO, 2001
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