Hostname: page-component-cb9f654ff-lqqdg Total loading time: 0 Render date: 2025-08-27T07:10:07.166Z Has data issue: false hasContentIssue false
  • English
  • Français

Magnetic observations of pulsating B and Be stars with ESPaDOnS and Narval

Published online by Cambridge University Press:  01 November 2008

James Silvester ,
C. Neiner ,
H. F. Henrichs ,
G. A. Wade ,
E. Alecian  and
V. Petit
James Silvester
Affiliation:
Department of Physics, Queen's University, Kingston, Ontario, Canada, K7L 3N6 Department of Physics, Royal Military College of Canada, Kingston, ON, Canada, K7K 7B4
C. Neiner
Affiliation:
GEPI, Observatoire de Paris, CNRS, 5 place Jules Janssen, 92190 Meudon, France
H. F. Henrichs
Affiliation:
Astronomical Institute “Anton Pannekoek”, University of Amsterdam, The Netherlands
G. A. Wade
Affiliation:
Department of Physics, Royal Military College of Canada, Kingston, ON, Canada, K7K 7B4
E. Alecian
Affiliation:
Department of Physics, Royal Military College of Canada, Kingston, ON, Canada, K7K 7B4
V. Petit
Affiliation:
Départment de physique, CRAQ, Université Laval, Québec, Canada, G1K 7P4
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.

Discoveries of magnetic fields in pulsating B and Be stars have been claimed from low-resolution spectropolarimetric observations with FORS1 at VLT. We used the new generation of high-resolution spectropolarimeters, ESPaDOnS at CFHT and NARVAL at TBL, to check for the existence of these fields. We find that most of the claimed magnetic stars do not host a magnetic field. This work shows the importance of a critical analysis of FORS1 data when searching for weak magnetic fields in early-type stars and the advantage of using ESPaDOnS and NARVAL to study such type of stars.

Keywords

Stars: magnetic fields – techniques: polarimetric – stars: early-type – stars: emission-line, Be

References

Alecian, E., Wade, G. A., Catala, C., et al. 2008, CoSka 38, 235Google Scholar
Donati, J.-F., Semel, M., Carter, B. D., Rees, D. E., & Collier, A. C. 1997, MNRAS 313, 658CrossRefGoogle Scholar
Hubrig, S., Briquet, M., Schöller, M., De Cat, P., Mathys, G., & Aerts, C. 2006, MNRAS 369, L61CrossRefGoogle Scholar
Hubrig, S., Yudin, R.V., Pogodin, M., Schőller, M., & Peters, G. J. 2007, AN 328, 1133Google Scholar
Henrichs, H. F., de Jong, J. A., Donati, J.-F., Catala, C., Wade, G. A., Shorlin, S. L. S., Veen, P. M., Nichols, J. S., & Kaper, L. 2000, The Be Phenomenon in Early-Type Stars, IAU Colloquium 175, ASP Conference Proceedings, Vol. 214, p.324CrossRefGoogle Scholar
Kupka, F., Piskunov, N. E., Ryabchikova, T. A., Stempels, H. C., & Wiess, W. W. 1999, A&AS 138, 119Google Scholar
Neiner, C., Geers, V. C., Henrichs, H. F., Floquet, M., Frémat, Y., Hubert, A.-M., Preuss, O., & Wiersema, K. 2003b, A&A 406, 1019Google Scholar
Neiner, C., Henrichs, H. F., Floquet, M., Frémat, Y., Preuss, O., Hubert, A.-M., Geers, V. C., Tijani, A. H., Nichols, J. S., & Jankov, S. 2003a, A&A 411, 565Google Scholar
Neiner, C., Hubert, A.-M., Frémat, Y. et al. 2003c, A&A 409, 275Google Scholar
Power, J., Wade, G. A., Aurière, M., Silvester, J., & Hanes, D. 2008, CoSka 38, 443Google Scholar