Astron. Astrophys. Suppl. Ser.
Volume 135, Number 2, March I 1999
|Page(s)||359 - 370|
|Published online||15 March 1999|
Recombination line intensities for hydrogenic ions: The fine-structure components of HI and HeII *
Particle Physics and Astronomy Research Council, Polaris House, North Star Avenue, Swindon, Wiltshire SN2 1SZ, UK
2 Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UK
Send offprint request to: P.J. Storey
Accepted: 21 October 1998
Emissivities have been calculated for fine-structure components of selected UV and optical recombination lines of HI and HeII. Results are given for a range of electron temperatures and densities, and in Cases A and B of Baker & Menzel (1938). Relative intensities, wavelengths and velocity shifts of the fine-structure components are tabulated. Applications to the spectra of gaseous nebulae are discussed. Depending on the temperature, density and Case, the centres of unresolved lines can shift by up to 0.9 km s-1 for HI and 3.3 km s-1 for HeII. A new calibration of the Hα–[NII] method for determining electron temperatures is given.
Key words: atomic data / line: formation / line: profiles / HII regions / planetary nebulae: general
All tables are also available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (188.8.131.52) or via http://cdsweb.u-strasbg.fr/Abstract.html
© European Southern Observatory (ESO), 1999