Hostname: page-component-cb9f654ff-mx8w7 Total loading time: 0 Render date: 2025-08-06T17:46:55.952Z Has data issue: false hasContentIssue false
  • English
  • Français

Pulsations in the late-type B supergiant star HD 202850†

Published online by Cambridge University Press:  18 February 2014

Sanja Tomić ,
Michaela Kraus  and
Mary Oksala
Sanja Tomić
Affiliation:
Department of Astronomy, Faculty of Mathematics, University of Belgrade Studentski trg 16, 11000 Belgrade, Serbia email: sanja@sunstel.asu.cas.cz
Michaela Kraus
Affiliation:
Astronomický ústav, Akademie věd České republiky Fričova 298, 25165 Ondřejov, Czech Republic
Mary Oksala
Affiliation:
Astronomický ústav, Akademie věd České republiky Fričova 298, 25165 Ondřejov, Czech Republic
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.

HD 202850 is a late B-type supergiant. It is known that photospheric lines of such stars vary. Due to macroturbulence the lines are much wider than expected. Macroturbulence has been linked to stellar pulsations. It has been reported that there are several B supergiants that undergo pulsations. In our previous work, we detected a pulsational period of 1.59 hours in this object from data taken with the Ondřejov 2-m telescope. We continued to investigate this object and we took several time series with the DAO 1.2-m telescope. Our new data suggest that there may be some additional pulsational periods in this star. We present our new results in this poster.

Keywords

stars: supergiantsoscillationslate-typetechniques: spectroscopicradial velocities

Information

Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Symposium S301: Precision Asteroseismology , August 2013 , pp. 503 - 504
Copyright
Copyright © International Astronomical Union 2014 

Footnotes

†

Based on observations acquired at the Dominion Astrophysical Observatory, Herzberg Institute of Astrophysics, National Research Council of Canada

References

Kraus, M., Tomić, S., Oksala, M. E., & Smole, M. 2012, A&A, 542, L32Google Scholar
Markova, N. & Puls, J. 2008, A&A, 478, 823Google Scholar
Saio, H. 2011, in: Neiner, C., Wade, G., Meynet, G., & Peters, G. (eds.), Active OB Stars: Structure, Evolution, Mass Loss, and Critical Limits, Proc. IAU Symposium No. 272 (Cambridge: Cambridge University Press) p. 468Google Scholar