Putting A Stars into Context: Evolution, Environment, and Related Stars
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Putting A Stars into Context: Evolution, Environment, and Related Stars

New paper registration

Abstract Deadline - April 10, 2013
Submitters Notified - May 3, 2013

Contributed talks will be selected from the submitted abstracts, and there will also be a poster session. All contributions will be included in the proceedings.

Your abstract should not contain more than 200 words. The word count does NOT include your title, authoring or cited references. For formulas, use LATEX.

One example.
Title: Non-LTE line formation for Pr II and Pr III in A and Ap stars
Authors: Mashonkina L., Institute of Astronomy, Russian Academy of Sciences, Moscow, Russia Ryabchikova T., Institute of Astronomy, Russian Academy of Sciences, Moscow, Russia
Ryabtsev A., Institute of Spectroscopy, Russian Academy of Sciences, Moscow, Russia
Abstract: Non-local thermodynamical equilibrium (non-LTE) line formation for singly-ionized and doubly-ionized praseodymium is considered for a range of effective temperatures between 7250~K and 9500~K. We evaluate the influence of departures from LTE on Pr abundance determinations and discuss the dependence of non-LTE effects on the atmospheric parameters. The Pr~II-Pr~III model atom is applied to determine the Pr abundance in the atmosphere of the roAp star HD\,24712 from the lines of two ionization stages. In the chemically uniform atmosphere with [Pr/H] = 3, the departures from LTE may explain only a small part (approximately 0.3~dex) of the difference between the LTE abundances derived from the Pr~II and Pr~III lines ($\simeq$2~dex). We find that the lines of both ionization stages are fitted for the vertical distribution of praseodymium, where the Pr enriched layer with [Pr/H] $\ge$ 4 exists in the outer atmosphere at $\log \tau_{5000} < -4$. The departures from LTE for Pr~II-Pr~III are strong in the stratified atmosphere and have the opposite sign for the Pr~II and Pr~III lines. Using the revised partition function of Pr~II and experimental transition probabilities, we determine the solar non-LTE abundance to be log (Pr/H)$_\odot = -11.15\pm0.08$.

MEANS OF SUBMISSION - ONLINE Please use this link http://astars2013.inasan.ru/abstract to submit your abstract for the Putting A Stars into Context: Evolution, Environment, and Related Stars Conference.

You will receive a confirmation email with your Abstract Submission Reference Number. Changes can be made to your abstract until the scoring process begins. Just return to your dashboard and select the Edit option under Abstracts. The edit option will no longer appear once scoring has commenced.
If you do not receive this confirmation email, please contact the secretariat using e-mail address astars2013@inasan.ru

Notification of programming decisions will come from the secretariat shortly after the expiry of deadlines and the working program will be posted to the web site. The notification will include specific presentation instructions.

The final program is published to this website and the abstracts to the web page http://astars2013.inasan.ru/abstract_book_final.pdf