Hostname: page-component-8448b6f56d-mp689 Total loading time: 0 Render date: 2024-04-23T08:58:47.857Z Has data issue: false hasContentIssue false
  • English
  • Français

Photometric Variability of OB-type stars as a New Window on Massive Stars

Published online by Cambridge University Press:  23 January 2015

M. Kourniotis ,
A. Z. Bonanos ,
I. Soszyński ,
R. Poleski ,
G. Krikelis  and
the OGLE team
M. Kourniotis
Affiliation:
IAASARS, National Observatory of Athens, GR-15236 Penteli, Greece email: mkourniotis@astro.noa.gr, bonanos@astro.noa.gr Section of Astrophysics, Astronomy and Mechanics, Faculty of Physics, University of Athens, Panepistimiopolis, GR15784 Zografos, Athens, Greece
A. Z. Bonanos
Affiliation:
IAASARS, National Observatory of Athens, GR-15236 Penteli, Greece email: mkourniotis@astro.noa.gr, bonanos@astro.noa.gr
I. Soszyński
Affiliation:
Warsaw University Observatory, Al. Ujazdowskie 4, 00-478 Warszawa, Poland
R. Poleski
Affiliation:
Warsaw University Observatory, Al. Ujazdowskie 4, 00-478 Warszawa, Poland Department of Astronomy, Ohio State University, 140 W. 18th Ave., Columbus, OH 43210, USA
G. Krikelis
Affiliation:
Section of Astrophysics, Astronomy and Mechanics, Faculty of Physics, University of Athens, Panepistimiopolis, GR15784 Zografos, Athens, Greece
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 present the first systematic study of 4646 spectroscopically confirmed early-type massive stars in the Small Magellanic Cloud (SMC), using variability as a tool to confine the physics of OB-type massive stars. We report the discovery of ∼100 massive eclipsing systems which are useful for the accurate determination of the fundamental parameters of massive stars and we evaluate the frequency of multiplicity. In addition, we explore the occurrence of the Oe/Be phenomenon and provide a large number of candidate non-radial pulsators, which can be further studied via asteroseismology. The results of this work (Kourniotis et al. 2014) will contribute to a better understanding of the role of metallicity in triggering processes associated to matter ejections and/or disk formation, which in turn affect mass loss and stellar rotation.

Keywords

stars: emission-lineBe(stars:) binaries: eclipsinggalaxies: individual (SMC)stars: variables: other
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Issue S307: New windows on massive stars: asteroseismology, interferometry, and spectropolarimetry , June 2014 , pp. 171 - 175
Copyright
Copyright © International Astronomical Union 2015 

References

Bonanos, A. Z., Lennon, D. J., Köhlinger, F., et al. 2010, AJ 140, 416Google Scholar
Graczyk, D. & Eyer, L. 2010, AcA 60, 109Google Scholar
Keller, S. C., Bessell, M. S., Cook, K. H., Geha, M., & Syphers, D. 2002, AJ 124, 2039Google Scholar
Kourniotis, M., Bonanos, A. Z., Soszyński, I., et al. 2014, A&A 562, A125Google Scholar
Rivinius, T., Carciofi, A. C., & Martayan, C. 2013, A&A Rev. 21, 69Google Scholar
Salmon, S., Montalbán, J., Morel, T., et al. 2012, MNRAS 422, 3460CrossRefGoogle Scholar
Sana, H., de Mink, S. E., de Koter, A., et al. 2012, Science 337, 444Google Scholar
Schwarzenberg-Czerny, A. 1989, MNRAS 241, 153Google Scholar
Udalski, A., Soszyński, I., Szymański, M. K., et al. 2008, AcA 58, 329Google Scholar
Vink, J. S., de Koter, A., & Lamers, H. J. G. L. M. 2001, A&A 369, 574Google Scholar