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Radiative Magnetic Reconnection in Astrophysics

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Magnetic Reconnection

Part of the book series: Astrophysics and Space Science Library ((ASSL,volume 427))

Abstract

In this chapter we review a new and rapidly growing area of research in high-energy plasma astrophysics—radiative magnetic reconnection, defined here as a regime of reconnection where radiation reaction has an important influence on the reconnection dynamics, energetics, and/or nonthermal particle acceleration. This influence be may be manifested via a variety of radiative effects that are critical in many high-energy astrophysical applications. The most notable radiative effects in astrophysical reconnection include radiation-reaction limits on particle acceleration, radiative cooling, radiative resistivity, braking of reconnection outflows by radiation drag, radiation pressure, viscosity, and even pair creation at highest energy densities. The self-consistent inclusion of these effects into magnetic reconnection theory and modeling sometimes calls for serious modifications to our overall theoretical approach to the problem. In addition, prompt reconnection-powered radiation often represents our only observational diagnostic tool available for studying remote astrophysical systems; this underscores the importance of developing predictive modeling capabilities to connect the underlying physical conditions in a reconnecting system to observable radiative signatures. This chapter presents an overview of our recent theoretical progress in developing basic physical understanding of radiative magnetic reconnection, with a special emphasis on astrophysically most important radiation mechanisms like synchrotron, curvature, and inverse-Compton. The chapter also offers a broad review of key high-energy astrophysical applications of radiative reconnection, illustrated by multiple examples such as: pulsar wind nebulae, pulsar magnetospheres, black-hole accretion-disk coronae and hot accretion flows in X-ray Binaries and Active Galactic Nuclei and their relativistic jets, magnetospheres of magnetars, and Gamma-Ray Bursts. Finally, this chapter discusses the most critical open questions and outlines the directions for future research of this exciting new frontier of magnetic reconnection research.

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Notes

  1. 1.

    Strictly speaking in weakly collisional plasmas this is not quite correct since the electron and ion outflow patterns are somewhat different, which results in an in-plane current circulation responsible for the quadrupole out-of-plane magnetic field.

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Acknowledgements

I am very grateful to the organizers of the Parker Workshop on Magnetic Reconnection in Brazil, March 2014, and especially to Dr. Walter Gonzalez. I am also indebted to Prof. Eugene Parker for being a constant shining inspiration.

I am also grateful to numerous colleagues for many stimulating and insightful conversations over many years on various topics discussed in this chapter. Specifically, I would like to thank M. Begelman, A. Beloborodov, A. Bhattacharjee, B. Cerutti, W. Daughton, E. de Gouveia dal Pino, J. Drake, D. Giannios, J. Goodman, R. Kulsrud, H. Li, N. Loureiro, Yu. Lyubarsky, M. Lyutikov, J. McKinney, M. Medvedev, K. Nalewajko, A. Spitkovsky, and G. Werner.

This work has been supported by NSF Grants PHY-0903851 and AST-1411879, DOE Grants DE-SC0008409 and DE-SC0008655, and NASA Grants NNX11AE12G, NNX12AP17G, NNX12AP18G, and NNX13AO83G.

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  1. Physics Department, Center for Integrated Plasma Studies, University of Colorado, Boulder, CO, 80309, USA

    D. A. Uzdensky

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  1. INPE, São José dos Campos, Brazil

    Walter Gonzalez

  2. University of Chicago, CHICAGO, Illinois, USA

    Eugene Parker

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Uzdensky, D.A. (2016). Radiative Magnetic Reconnection in Astrophysics. In: Gonzalez, W., Parker, E. (eds) Magnetic Reconnection. Astrophysics and Space Science Library, vol 427. Springer, Cham. https://doi.org/10.1007/978-3-319-26432-5_12

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