Magnetic Fields in Galaxies

Rainer Beck

doi:10.1017/9781316160916.006

5 - Magnetic Fields in Galaxies

Published online by Cambridge University Press: 21 April 2018

Rainer Beck

Edited by

Jorge Sánchez Almeida and

María Jesús Martínez González

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Rainer Beck: Affiliation:
Max Planck Institut für Radioastronomie, Germany
Jorge Sánchez Almeida: Affiliation:
Instituto de Astrofísica de Canarias, Tenerife
María Jesús Martínez González: Affiliation:
Instituto de Astrofísica de Canarias, Tenerife

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Summary

Introduction

Magnetism is a fundamental force with special properties.

• Most baryonic matter is ionized. Magnetic fields are easy to generate.

• Magnetic monopoles do not exist or are extremely rare. Magnetic fields are hard to destroy.

• Magnetic fields need illumination. Magnetic fields are difficult to observe.

The scarceness of data leaves many questions on cosmic magnetic fields.

• When and how were the first fields generated?

• Did significant fields exist before galaxies formed?

• How and how fast were the fields amplified?

• How did fields affect the evolution of stars, planets, galaxies and galaxy clusters?

• How strongly is intergalactic space magnetized?

Magnetic fields are often ignored in astrophysics, in particular in models of galaxies and the interstellar medium (ISM), although they are a major agent in the ISM and in galaxy halos, and important for the structure and evolution of galaxies.

• Magnetic fields contribute significantly to the total pressure which balances the gas disk of galaxies against gravitation (Fletcher & Shukurov, 2001).

• Magnetic turbulence distributes energy from supernova explosions within the ISM (Subramanian, 1998).

• Magnetic reconnection is a possible heating source for the ISM and halo gas (Birk et al., 1998).

• Magnetic fields increase angular momentum transport and hence the gas inflow rate in barred galaxies (Beck et al., 2005; Kim & Stone, 2012).

• Magnetic fields affect the dynamics of the turbulent ISM (de Avillez & Breitschwerdt, 2005) and the gas flows in spiral arms (Gómez & Cox, 2002).

• Magnetic fields make the gaseous spiral arms more patchy and drive gas outflows into the halo (Pakmor & Springel, 2013).

• The shock strength in spiral density waves is decreased and structure formation is reduced in the presence of strong fields (Dobbs & Price, 2008; Fletcher et al., 2011).

• Magnetic fields stabilize gas clouds and reduce the star-formation efficiency to the observed low values (Vázquez-Semadeni et al., 2005; Price & Bate, 2008).

• Magnetic fields are essential for the onset of star formation as they enable the removal of angular momentum from the protostellar cloud via ambipolar diffusion (Heitsch et al., 2004).

Type: Chapter
Information: Cosmic Magnetic Fields
, pp. 123 - 160

DOI: https://doi.org/10.1017/9781316160916.006 [Opens in a new window]

Publisher: Cambridge University Press

Print publication year: 2018

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