Volume 559, November 2013
|Number of page(s)||8|
|Section||Atomic, molecular, and nuclear data|
|Published online||15 November 2013|
Blue satellites on He lines due to He-He collisions⋆
Observatoire de Paris, GEPI, UMR 8111, CNRS, Université Paris VII, 61
avenue de l’Observatoire,
2 Institut d’Astrophysique de Paris, UMR 7095, CNRS, Université Paris VI, 98bis Boulevard Arago, Paris, France
3 Laboratoire de Physique et Chimie Quantique, Université de Toulouse (UPS) and CNRS, 118 route de Narbonne, 31400 Toulouse, France
4 Department of Physics and Astronomy, University of Louisville, Louisville, Kentucky 40292, USA
Accepted: 3 September 2013
The shape and broadening of He lines affects radiative transport in dense, He-rich, stellar atmospheres. At wavelengths inaccessible for direct observation, we rely on theoretical calculations of self-broadening to support stellar structure and spectral modeling. In this work, we examine lines of He due to 1s–2p and 2p–3s transitions. The line profiles are analyzed in terms of a unified theory of spectral line broadening using ab initio potential energies that have been recently determined. For temperatures up to 20 000 K, the linear dependence of width and shift on gas density and the non-linear dependence on temperature of the Lorentzian core of the resonance line are described. Beyond the conventional symmetrical Lorentzian core, we show that they are asymmetrical and have significant additional contributions on the short wavelength side. This blue asymmetry is a consequence of maxima in the corresponding He2 potential energy difference curves at short and intermediate internuclear distance. Over a limited range of density and temperature, laboratory measurements in the visible and near infrared can be used to validate the potentials that underlie the spectral line profile theory, which is useful for modeling spectra over the extreme ranges of temperature and density encountered in stellar and planetary atmospheres.
Key words: line: profiles / stars: atmospheres / brown dwarfs / white dwarfs
Data of Fig. 6 are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (126.96.36.199) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/559/A70
© ESO, 2013
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