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Magnetic fields in AGB stars and (proto-) Planetary Nebulae

Published online by Cambridge University Press:  01 November 2008

Fabrice Herpin
Affiliation:
Université de Bordeaux, Lab. d'Astrophysique de Bordeaux, F-33000 Bordeaux, France email: herpin@obs.u-bordeaux1.fr CNRS/INSU, UMR 5804, BP 89, 33271 FLOIRAC cedex, France
A. Baudy
Affiliation:
Université de Bordeaux, Lab. d'Astrophysique de Bordeaux, F-33000 Bordeaux, France email: herpin@obs.u-bordeaux1.fr CNRS/INSU, UMR 5804, BP 89, 33271 FLOIRAC cedex, France
E. Josselin
Affiliation:
GRAAL, Université Montpellier II - ISTEEM, CNRS, Place Eugène Bataillon, F-34095 Montpellier Cedex, France
C. Thum
Affiliation:
Institut de Radio Astronomie Millimétrique, 300 rue de la Piscine, F-38406 Saint Martin d'Hères, France
H. Wiesemeyer
Affiliation:
Institut de Radio Astronomie Millimétrique, 300 rue de la Piscine, F-38406 Saint Martin d'Hères, France
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Abstract

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During its quick transition to the Planetary Nebula stage, the Asymptotic Giant Branch star will completely change its geometry. This AGB stellar evolution stage is characterized by a high mass loss driven by the radiation pressure. Strong magnetic field may rule the mass loss geometry and the global shaping of these objects. Following our previous work on the polarization of the SiO maser emission in a representative sample of O-rich evolved stars, we present here a study towards C-rich objects and PPN/PN objects to obtain unbiased conclusions. Using Xpol at the IRAM-30 m telescope, we have conducted CN N=1-0 observations to investigate the Zeeman effect in this molecule and draw conclusion on the evolution of the magnetic field and its influence during the transition of an AGB star to the PN stage. Following the analysis described by Crutcher et al. (1996) we derive an estimate of the magnetic field.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2009

References

Bachiller, R. et al. 1997a, A&A 319, 235Google Scholar
Bachiller, R. et al. 1997b, A&A 324, 1123Google Scholar
Bujarrabal, V., Castro-Carrizo, A., Alcolea, J., & Sánchez Contreras, C. 2001, A&A 377, 868Google Scholar
Crutcher, R. M. et al. 1996, ApJ 456, 217CrossRefGoogle Scholar
Elitzur, M. 1996, ApJ 457, 415CrossRefGoogle Scholar
Herpin, F., Baudry, A., Thum, C., Morris, D., & Wiesemeyer, H. 2006, A&A 450, 667Google Scholar
Huggins, P. J. & Glassgold, A. E. 1982, AJ 87, 1828CrossRefGoogle Scholar
Jordan, S., Werner, K., & O'Toole, S. J. 2005, A&A 432, 273Google Scholar
Josselin, E. & Bachiller, R. 2003, A&A 397, 659Google Scholar
Kemball, A. J. & Diamond, P. J. 1997 ApJ 481, L111CrossRefGoogle Scholar
Kwok, S. 2000, in The origin and Evolution of Planetary Nebulae, Cambridge Astrophysics Series 31, Cambridge University Press editionCrossRefGoogle Scholar
Lindqvist, M. et al. 2000, A&A 361, 1036Google Scholar
Lucas, R. et al. 1995, Ap&SS 224, 293Google Scholar
Nyman, L.-A., Hall, P. J., & Olofsson, H. 1998 A&ASS 127, 185200Google Scholar
Sahai, R. & Trauger, J. T. 1998, AJ 116, 1357CrossRefGoogle Scholar
Soker, N. 2002, MNRAS 337, 1038CrossRefGoogle Scholar
Szczerba, R. et al. 2002, A&A 381, 491Google Scholar
Szymczak, M. & Cohen, R. J. 1997, MNRAS 288, 945CrossRefGoogle Scholar
Thum, C., Wiesemeyer, H., Morris, D., Navarro, S., & Torres, M. 2003 SPIE 4843, 272Google Scholar
Thum, C. et al. 2008, PASP 120, 777CrossRefGoogle Scholar
Vlemmings, W., Diamond, P. J., & van Langevelde, H. J. 2001, A&A 375, L1Google Scholar