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5 - Magnetic Fields in Galaxies

Published online by Cambridge University Press:  21 April 2018

By
Rainer Beck
Edited by
Jorge Sánchez Almeida  and
María Jesús Martínez González
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
    Publisher: Cambridge University Press
    Print publication year: 2018

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    To save content items to your account, please confirm that you agree to abide by our usage policies. If this is the first time you use this feature, you will be asked to authorise Cambridge Core to connect with your account. Find out more about saving content to Google Drive.

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