Hostname: page-component-78c5997874-t5tsf Total loading time: 0 Render date: 2024-11-19T03:41:55.379Z Has data issue: false hasContentIssue false
  • English
  • Français

Magnetism in the nearby galaxy M 33

Published online by Cambridge University Press:  01 November 2008

F. S. Tabatabaei ,
M. Krause ,
R. Beck  and
A. Fletcher
F. S. Tabatabaei
Affiliation:
Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany email: [email protected], [email protected], [email protected]
M. Krause
Affiliation:
Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany email: [email protected], [email protected], [email protected]
R. Beck
Affiliation:
Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany email: [email protected], [email protected], [email protected]
A. Fletcher
Affiliation:
School of Mathematics and Statistics, Newcastle University, Newcastle upon Tyne, NE1 7RU, U.K., email: [email protected]
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.

Using high-resolution data of the linearly polarized intensity and polarization angle at 3.6, 6.2, and 20 cm together with a 3-D model of the regular magnetic field, we study variations of the structure, strength, and energy density of the magnetic field in the Scd galaxy M 33. The regular magnetic field consists of a horizontal component (represented by an axisymmetric mode from 1 to 3 kpc radius and a superposition of axisymmetric and bisymmetric modes from 3 to 5 kpc radius) and a vertical component. However, the inferred ‘vertical field’ may be partly due to a galactic warp. We estimate the average total and regular magnetic field strengths as ≃6.4 and 2.5 μG, respectively. Generation of interstellar magnetic fields by turbulent gas motion in M 33 is indicated as the turbulent and magnetic energy densities are about equal.

Keywords

Galaxies: individual: M33 – radio continuum: galaxies – galaxies: magnetic field – galaxies: ISM
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Symposium S259: Cosmic Magnetic Fields: From Planets, to Stars and Galaxies , November 2008 , pp. 545 - 546
Copyright
Copyright © International Astronomical Union 2009

References

Beck, R. 1979, Ph.D. Thesis, Rheinische Friedrich-Wilhelms-Universitaet, BonnGoogle Scholar
Berkhuijsen, E. M., Horellou, C., Krause, M., Neininger, N., et al. 1997, A&A 318, 700Google Scholar
Buczilowski, U. R. & Beck, R. 1991, A&A 241, 47Google Scholar
Fletcher, A., Berkhuijsen, E. M., Beck, R., & Shukurov, A. 2004, A&A 414, 53Google Scholar
Tabatabaei, F. S., Krause, M., & Beck, R. 2007a, A&A 472, 785Google Scholar
Tabatabaei, F. S., Beck, R., Krügel, E., Krause, M., Berkhuijsen, , et al. 2007b, A&A 475, 133Google Scholar
Tabatabaei, F. S., Krause, M., Fletcher, A., & Beck, R. 2008, A&A 490, 1005Google Scholar