Hostname: page-component-78c5997874-4rdpn Total loading time: 0 Render date: 2024-11-14T11:57:18.643Z Has data issue: false hasContentIssue false
  • English
  • Français

On the new late B- and early A-type periodic variable stars

Published online by Cambridge University Press:  18 February 2014

Nami Mowlavi ,
Sophie Saesen ,
Fabio Barblan  and
Laurent Eyer
Nami Mowlavi
Affiliation:
Geneva Observatory, University of Geneva, 51 chemin des Maillettes, 1290 Versoix, Switzerland email: Nami.Mowlavi@unige.ch
Sophie Saesen
Affiliation:
Geneva Observatory, University of Geneva, 51 chemin des Maillettes, 1290 Versoix, Switzerland email: Nami.Mowlavi@unige.ch
Fabio Barblan
Affiliation:
Geneva Observatory, University of Geneva, 51 chemin des Maillettes, 1290 Versoix, Switzerland email: Nami.Mowlavi@unige.ch
Laurent Eyer
Affiliation:
Geneva Observatory, University of Geneva, 51 chemin des Maillettes, 1290 Versoix, Switzerland email: Nami.Mowlavi@unige.ch
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We summarize the properties of the new periodic, small-amplitude, variable stars recently discovered in the open cluster NGC 3766. They are located in the region of the Hertzsprung-Russell diagram between δ Sct and slowly pulsating B stars, a region where no sustained pulsation is predicted by standard models. The origin of their periodic variability is currently unknown. We also discuss how the Gaia mission, launched at the end of 2013, can contribute to our knowledge of those stars.

Keywords

open clusters: NGC 3766stars: variablesstars: pulsations
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Symposium S301: Precision Asteroseismology , August 2013 , pp. 43 - 46
Copyright
Copyright © International Astronomical Union 2014 

References

Christensen-Dalsgaard, J. 2004, in: Danesy, D. (ed.), SOHO 14 Helio- and Asteroseismology: Towards a Golden Future, ESA SP-559, p. 1Google Scholar
Eyer, L. & Mignard, F. 2005, MNRAS, 361, 1136CrossRefGoogle Scholar
Eyer, L., Mowlavi, N., Varadi, M., et al. 2009, in: Heydari-Malayeri, M., Reyl, C. and Samadi, R., (eds.), Proceedings of the Annual meeting of the French Society of Astronomy and Astrophysics, SF2A-2009, p. 45Google Scholar
Jordi, C., Gebran, M., Carrasco, J. M., et al. 2010, A&A, 523, 48Google Scholar
Mowlavi, N., Barblan, F., Saesen, S., & Eyer, L. 2013, A&A 554, A108 (MBSE13)Google Scholar
Mowlavi, N., Saesen, S., Barblan, F., & Eyer, L. 2014, in: Putting A Stars into Context: Evolution, Environment, and Related Stars (June 3-7, 2013, Moscow), Press-Menu, in press (arXiv: 1310.6488)Google Scholar
Pamyatnykh, A. A. 1999, AcA, 49, 119Google Scholar
Townsend, R. H. D. 2005, MNRAS, 364, 573Google Scholar
Ushomirsky, G. & Bildsten, L. 1998, ApJ, 497, L101Google Scholar