Volume 499, Number 3, June I 2009
|Page(s)||879 - 890|
|Published online||29 April 2009|
Model atmospheres of chemically peculiar stars
Self-consistent empirical stratified model of HD 24712
Institute of Astronomy, Vienna University, Turkenschanzstrasse 17, 1180 Vienna, Austria e-mail: firstname.lastname@example.org
2 Institute of Astronomy, Russian Academy of Science, Pyatnitskaya 48, 119017 Moscow, Russia
3 Department of Astronomy and Space Physics, Uppsala University, Box 515, 751 20 Uppsala, Sweden
Accepted: 19 March 2009
Context. High-resolution spectra of some chemically peculiar stars clearly demonstrate the presence of strong abundance gradients in their atmospheres. However, these inhomogeneities are usually ignored in the standard scheme of model atmosphere calculations, breaking the consistency between model structure and spectroscopically derived abundance pattern.
Aims. In this paper we present the first empirical self-consistent stellar atmosphere model of the roAp star HD 24712 with stratification of chemical elements included, and which is derived directly from the observed profiles of spectral lines without time-consuming simulations of physical mechanisms responsible for these anomalies.
Methods. We used the LLmodels stellar model atmosphere code and DDAFIT minimization tool for analysis of chemical element stratification and construction of a self-consistent atmospheric model. Empirical determination of Pr and Nd stratification in the atmosphere of HD 24712 is based on NLTE line formation for Pr ii/iii and Nd ii/iii with the use of the DETAIL code.
Results. Based on an iterative procedure of stratification analysis and subsequent re-calculation of model atmosphere structure, we constructed a self-consistent model of HD 24712, i.e. the model whose temperature-pressure structure is consistent with the results of the stratification analysis. It is shown that stratification of chemical elements leads to considerable changes in model structure compared to the non-stratified homogeneous case. We find that accumulation of rare earth elements (REE) allows for the inverse temperature gradient to be present in the upper atmosphere of the star with a maximum temperature increase of about 600 K.
© ESO, 2009
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.