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Galactic and Extragalactic Magnetic Fields

  • Conference paper
The Astrophysics of Galactic Cosmic Rays

Part of the book series: Space Sciences Series of ISSI ((SSSI,volume 13))

Abstract

The current state of research of the Galactic magnetic field is reviewed critically. The average strength of the total field derived from radio synchrotron data, under the energy equipartition assumption, is 6±2 μG locally and about 10±3 μG at 3 kpc Galactic radius. These values agree well with the estimates using the locally measured cosmic-ray energy spectrum and the radial variation of protons derived from γ-rays. Optical and synchrotron polarization data yield a strength of the local regular field of 4 ± 1 μG, but this value is an upper limit if the field strength fluctuates within the beam or if anisotropic fields are present. Pulsar rotation measures, on the other hand, give only 1.4 ± 0.2 μG, a lower limit if fluctuations in regular field strength and thermal electron density are anticorrelated along the pathlength. The local regular field may be part of a ‘magnetic arm’ between the optical arms. However, the global structure of the regular Galactic field is not yet known. Several large-scale field reversals in the Galaxy were detected from rotation measure data, but a similar phenomenon was not observed in external galaxies. The Galactic field may be young in terms of dynamo action so that reversals from the chaotic seed field are preserved, or a mixture of dynamo modes causes the reversals, or the reversals are signatures of large-scale anisotropic field loops. The Galaxy is surrounded by a thick disk of radio continuum emission of similar extent as in edge-on spiral galaxies. While the local field in the thin disk is of even symmetry with respect to the plane (quadrupole), the global thick-disk field may be of dipole type. The Galactic center region hosts highly regular fields of up to milligauss strength which are oriented perpendicular to the plane. A major extension of the data base of pulsar rotation measures and Zeeman splitting measurements is required to determine the structure of the Galactic field. Further polarization surveys of the Galactic plane at wavelengths of 6 cm or shorter may directly reveal the fine structure of the local magnetic field.

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Authors and Affiliations

  1. Max-Planck-Institut für Radioastronomie, D-53121, Auf dem Hügel 69, Bonn, Germany

    Rainer Beck

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  1. Rainer Beck
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Editors and Affiliations

  1. Max-Planck-Institut für Extraterrestrische Physik, Garching, Germany

    Roland Diehl

  2. Institut de Physique Nucléaire d’Orsay, IN2P3-CNRS / Université Paris/Sud, Orsay, France

    Etienne Parizot

  3. International Space Science Institute, Bern, Switzerland

    Reinald Kallenbach  & Rudolf Von Steiger  & 

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Beck, R. (2001). Galactic and Extragalactic Magnetic Fields. In: Diehl, R., Parizot, E., Kallenbach, R., Von Steiger, R. (eds) The Astrophysics of Galactic Cosmic Rays. Space Sciences Series of ISSI, vol 13. Springer, Dordrecht. https://doi.org/10.1007/978-94-017-3239-0_21

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  • DOI: https://doi.org/10.1007/978-94-017-3239-0_21

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