Hostname: page-component-8448b6f56d-sxzjt Total loading time: 0 Render date: 2024-04-23T08:19:37.327Z Has data issue: false hasContentIssue false
  • English
  • Français

Magnetism in Herbig Ae/Be stars and the link to the Ap/Bp stars

Published online by Cambridge University Press:  03 November 2009

C. Neiner ,
J.-P. Zahn ,
E. Alecian ,
C. Catala ,
G.A. Wade ,
S. Bagnulo ,
T. Boehm ,
J.-C. Bouret ,
J.-F. Donati  and
C. Folsom
...Show all authors
E. Alecian
Affiliation:
LESIA (Observatoire de Paris), France Royal Military College, Canada
C. Catala
Affiliation:
LESIA (Observatoire de Paris), France
G.A. Wade
Affiliation:
Royal Military College, Canada
S. Bagnulo
Affiliation:
Armagh Observatory, UK
T. Boehm
Affiliation:
LATT (Observatoire Midi-Pyrénées), France
J.-C. Bouret
Affiliation:
Laboratoire d'Astrophysique de Marseille, France
J.-F. Donati
Affiliation:
LATT (Observatoire Midi-Pyrénées), France
C. Folsom
Affiliation:
Armagh Observatory, UK
J. Grunhut
Affiliation:
LESIA (Observatoire de Paris), France
J.D. Landstreet
Affiliation:
University of Western Ontario, Canada
S.C. Marsden
Affiliation:
Anglo-Australian Observatory, Australia
P. Petit
Affiliation:
LATT (Observatoire Midi-Pyrénées), France
J. Ramirez
Affiliation:
Royal Military College, Canada
J. Silvester
Affiliation:
LESIA (Observatoire de Paris), France
Get access

Abstract

Among the A/B stars, about 5% host large-scale organised magnetic fields. These magnetic stars show also abundance anomalies in their spectra, and are therefore called the magnetic Ap/Bp stars. Most of these stars are also slow rotators compared to the normal A and B stars. Today, one of the greatest challenges concerning the Ap/Bp stars is to understand the origin of their slow rotation and their magnetic fields. The favoured hypothesis for the latter is that the fields are fosils, which implies that the magnetic fields subsist throughout the different evolutionary phases, and in particular during the pre-main sequence phase. The existence of magnetic fields at the pre-main sequence phase is also required to explain the slow rotation of Ap/Bp stars. 
During the last 3 years we performed a spectropolarimetric survey of the Herbig Ae/Be stars in the field and in young clusters, in order to investigate their magnetism and rotation. These investigations have resulted in the detection and/or confirmation of magnetic fields in 8 Herbig Ae/Be stars, ranging in mass from 2 to nearly 15 solar masses. In this paper I will present the results of our survey, as well as their implications for the origin and evolution of the magnetic fields and rotation of the A and B stars.

Type
Research Article
Information
European Astronomical Society Publications Series , Volume 39: Stellar Magnetism , 2009 , pp. 121 - 132
Copyright
© EAS, EDP Sciences, 2009

Access options

Get access to the full version of this content by using one of the access options below. (Log in options will check for institutional or personal access. Content may require purchase if you do not have access.)

References

Alecian, E., Catala, C., Wade, G.A., et al., 2008a, MNRAS, 385, 391
Alecian, E., Wade, G.A., Catala, C., et al., 2008b, A&A, 481, 99
Bouret, J.-C., Catala, C., & Simon, T., 1997, A&A, 328, 606
Catala, C., Alecian, E., Donati, J.-F., et al., 2007, A&A, 462, 293
Catala, C., Böhm, T., Donati, J.-F., & Semel, M., 1993, A&A, 278, 187 PubMed
Catala, C., Simon, T., Praderie, F., et al., 1989, A&A, 221, 273
Claret, A., 2000, A&A, 363, 1081
de Winter, D., Koulis, C., Thé, P.S., et al., 1997, A&AS, 121, 223
Donati, J.-F., Semel, M., Carter, B.D., et al., 1997, MNRAS, 291, 658
Eisner, J.A., Lane, B.F., Akeson, R.L., et al., 2003, ApJ, 588, 360
Folsom, C.P., Wade, G.A., Kochukhov, O., et al., 2008, MNRAS, 391, 901
Gray, D.F., 1992, The observation and analysis of stellar photospheres, Cambridge Astrophysics Series, 2nd ed. (Cambridge: Cambridge University Press)
Hamaguchi, K., Yamauchi, S., & Koyama, K., 2005, ApJ, 618, 360 CrossRef
Hubrig, S., Schöller, M., & Yudin, R.V., 2004, A&A, 428, L1
Landi degl'Innocenti, E., & Landi degl'Innocenti, M., 1973, Sol. Phys., 31, 299 CrossRef
Lignières, F., Catala, C., & Mangeney, A., 1996, A&A, 314, 465
Morel, P., 1997, A&AS, 124, 597
Muzerolle, J., Calvet, N., & Hartmann, L., 2001, ApJ, 550, 944 CrossRef
Muzerolle, J., D'Alessio, P., Calvet, N., & Hartmann, L., 2004, ApJ, 617, 406 CrossRef
Natta, A., Prusti, T., Neri, R., et al., 2001, A&A, 371, 186
Palla, F., & Stahler, S.W., 1993, ApJ, 418, 414 CrossRef
Park, B.-G., & Sung, H., 2002, AJ, 123, 892 CrossRef
Park, B.-G., Sung, H., Bessell, M.S., & Kang, Y.H., 2000, AJ, 120, 894 CrossRef
Royer, F., Zorec, J., & Gómez, A.E., 2007, A&A, 463, 671
Semel, M., Donati, J.-F., & Rees, D.E., 1993, A&A, 278, 231
Stępień, K., 2000, A&A, 353, 227
Thé, P.S., de Winter, D., & Perez, M.R., 1994, A&AS, 104, 315
Vieira, S.L.A., Corradi, W.J.B., Alencar, S.H.P., et al., 2003, AJ, 126, 2971 CrossRef
Vink, J.S., Drew, J.E., Harries, T.J., & Oudmaijer, R.D., 2002, MNRAS, 337, 356 CrossRef
Wade, G.A., Bagnulo, S., Drouin, D., et al., 2007, MNRAS, 376, 1145
Wade, G.A., Drouin, D., Bagnulo, S., et al., 2005, A&A, 442, L31