Volume 464, Number 2, March III 2007
|Page(s)||715 - 734|
|Published online||02 January 2007|
The He Fowler lines and the O and N Bowen fluorescence lines in the symbiotic nova RR Telescopii
INAF – Osservatorio Astronomico di Trieste, via Tiepolo 11, 34143 Trieste, Italy e-mail: email@example.com
2 CIFIST Marie Curie Excellence Team
3 Observatoire de Paris, GEPI, 5 place Jules Janssen, 92195 Meudon, France
Accepted: 17 December 2006
Aims.A detailed study of the and Bowen lines in the spectrum of RR Tel.
Methods.Absolute intensities for the , , and emission lines have been obtained from STIS, UVES, FEROS and IUE data, after re-calibration of UVES and FEROS on the STIS scale.
Results.A new measure of reddening ( ~ 0.00) has been obtained from the comparison between the observed and the theoretical intensity decrement for 20 emission lines of the Fowler (n 3) series. This value has been confirmed by the STIS and IUE continuum distribution, and by the value of nH from the damped profile of the IS H Ly-α line. We have obtained very accurate measurements for about thirty Bowen lines of and a precise determination of the efficiency in the O1 and O3 excitation channels (18% and 0.7%, respectively). The relative intensities are in good agreement with the predictions by Froese Fischer (1994). A detailed study of the decays from all levels involved in the Bowen mechanism has lead to the detection of two new Bowen lines near λ 2190. High resolution IUE data have shown a nearly linear decline with time, from 1978 to 1995, in the efficiency of the O1 and O3 processes, with a steeper slope for the O3 channel. A detailed study of the λ 4640 lines and of their excitation mechanism has shown that, recombination and continuum fluorescence being ruled out, line fluorescence remains the only viable mechanism to pump the 3d and 3d levels of . We point out the important role of multiple scattering in the resonance lines of and near λ 374 and show that the observed line ratios and intensities can be explained in terms of line fluorescence by the three resonance lines of at λλ 374.432, 374.162 and 374.073 under optically thick conditions.
Key words: stars: novae, cataclysmic variables / stars: binaries: symbiotic / ultraviolet: stars / atomic processes / radiative transfer
© ESO, 2007
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.