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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

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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

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