Volume 423, Number 1, August III 2004
|Page(s)||335 - 340|
|Section||Stellar structure and evolution|
|Published online||29 July 2004|
On the crossing mode of the long-period Cepheid SV Vulpeculae
Department of Astronomy and Physics, Saint Mary's University, Halifax, Nova Scotia B3H 3C3, Canada e-mail: firstname.lastname@example.org
2 Sternberg Astronomical Institute and Isaac Newton Institute of Chile, Moscow Branch, 13 Universitetskij prosp., Moscow 119899, Russia e-mail: email@example.com
Accepted: 5 May 2004
The Cepheid SV Vul is demonstrated to be in the second crossing of the instability strip on the basis of its well-defined period decrease of -214.3 ± 5.5 s yr-1. Recent arguments from its atmospheric abundance pattern that it is in the first crossing are not supported by the historical photometric data. Furthermore, an examination of atmospheric abundance patterns for other Cepheids in advanced strip crossing modes suggests that the presence of CNO-processed material in the atmospheres of intermediate-mass stars does not arise from red supergiant dredge-up phases but from meridional mixing during previous evolution as rapidly-rotating main-sequence B-type stars.
Key words: stars: variables: Cepheids / stars: abundances / stars: evolution
© ESO, 2004
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.