Hostname: page-component-586b7cd67f-2brh9 Total loading time: 0 Render date: 2024-11-28T02:32:02.704Z Has data issue: false hasContentIssue false
  • English
  • Français

A Search for White Dwarf Companions of Be Stars

Published online by Cambridge University Press:  07 August 2017

A.J.M. Piters ,
E.J.A. Meurs ,
J. Coté ,
M.H. Van Kerkwijk ,
J. Van Paradijs ,
O.R. Pols  and
L.B.F.M. Waters
A.J.M. Piters
Affiliation:
1) Astr. Institute “Anton Pannekoek”, Amsterdam, The Netherlands, & Center for High-Energy Astroph., Amsterdam, The Netherlands
E.J.A. Meurs
Affiliation:
2) Max Planck Institut für Extraterrestrische Physik, Garching bei München, Germany
J. Coté
Affiliation:
1) Astr. Institute “Anton Pannekoek”, Amsterdam, The Netherlands, & Center for High-Energy Astroph., Amsterdam, The Netherlands
M.H. Van Kerkwijk
Affiliation:
1) Astr. Institute “Anton Pannekoek”, Amsterdam, The Netherlands, & Center for High-Energy Astroph., Amsterdam, The Netherlands
J. Van Paradijs
Affiliation:
1) Astr. Institute “Anton Pannekoek”, Amsterdam, The Netherlands, & Center for High-Energy Astroph., Amsterdam, The Netherlands
O.R. Pols
Affiliation:
1) Astr. Institute “Anton Pannekoek”, Amsterdam, The Netherlands, & Center for High-Energy Astroph., Amsterdam, The Netherlands
L.B.F.M. Waters
Affiliation:
3) SRON Laboratory for Space Research, Groningen, The Netherlands

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.

Preliminary results of an extended multi-wavelength study of bright B- and Be-type stars are presented. This project aims at finding evidence for the existence of white-dwarf companions to Be stars which are predicted as the result of close binary evolution. Comparison of ROSAT all-sky survey data with simultaneous measurements of Hα profiles and infrared photometry suggests that there is no difference in the X-ray behaviour of Be stars with respect to that of normal B stars. The ROSAT X-ray luminosities of B and Be stars range from 10−8 to 10−5 times the bolometric luminosity.

Type
Oral and Contributed Papers
Information
Symposium - International Astronomical Union , Volume 151: Evolutionary Processes in Interacting Binary Stars , 1992 , pp. 347 - 350
Copyright
Copyright © Kluwer 1992 

References

Dougherty, S.M., Taylor, A.R., and Clark, T.A. (1991), Astron. J. , in press Google Scholar
Friend, D.B., and MacGregor, K.B. (1984), Astrophys. J. 282, 591 Google Scholar
van den Heuvel, E.P.J., and Rappaport, S. (1987), in Proc. IAU Symposium 98, “Physics of Be Stars”, Eds. Slettebak, A. and Snow, T.P., p. 291 Google Scholar
Pallavicini, R., Golub, L., Rosner, R., Vaiana, G.S., Ayres, T., and Linsky, J.L. (1981), Astrophys. J. 248, 279 Google Scholar
Pols, O.R., Coté, J., Waters, L.B.F.M., and Heise, J. (1991), Astron. Astroph. 241, 419 Google Scholar
Waters, L.B.F.M. (1989), in: Proceedings of the 23rd ESLAB Symposium, ESA SP-296 (Vol. 1), p. 25 Google Scholar
Waters, L.B.F.M., Pols, O.R., Hogeveen, S.J., Coté, J., van den Heuvel, E.P.J. (1989), Astron. Astrophys. 220, L1 Google Scholar