Magnetic Reconnection in Astrophysical and Laboratory Plasmas

Zweibel, Ellen G.; Yamada, Masaaki

doi:10.1146/annurev-astro-082708-101726

Cited by 530 publications

(454 citation statements)

References 212 publications

(176 reference statements)

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“…Rapid reconnection of magnetic fields of different topologies may happen in spontaneous current sheets or be due to an external driving force (see, e.g., Zweibel and Yamada 2009). Mechanisms of direct acceleration of charged particles by the reconnecting magnetic field were studied in detail both analytically and numerically (see, e.g., Zelenyi et al 1990, Hoshino 2005, Birn and Priest 2007, Drake et al 2006, Pritchett 2006, Lazarian and Opher 2009, Artemyev et al 2013, Birn et al 2012.…”

Section: Particle Acceleration and Non-thermal Radiation In Starburstmentioning

confidence: 99%

Nonthermal particles and photons in starburst regions and superbubbles

Bykov

2014

Astron Astrophys Rev

118

102

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Starforming factories in galaxies produce compact clusters and loose associations of young massive stars. Fast radiation-driven winds and supernovae input their huge kinetic power into the interstellar medium in the form of highly supersonic and superalfvenic outflows. Apart from gas heating, collisionless relaxation of fast plasma outflows results in fluctuating magnetic fields and energetic particles. The energetic particles comprise a long-lived component which may contain a sizeable fraction of the kinetic energy released by the winds and supernova ejecta and thus modify the magnetohydrodynamic flows in the systems. We present a concise review of observational data and models of nonthermal emission from starburst galaxies, superbubbles, and compact clusters of massive stars. Efficient mechanisms of particle acceleration and amplification of fluctuating magnetic fields with a wide dynamical range in starburst regions are discussed. Sources of cosmic rays, neutrinos and multi-wavelength nonthermal emission associated with starburst regions including potential galactic "PeVatrons" are reviewed in the global galactic ecology context.

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Section: Particle Acceleration and Non-thermal Radiation In Starburstmentioning

confidence: 99%

Nonthermal particles and photons in starburst regions and superbubbles

Bykov

2014

Astron Astrophys Rev

118

102

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“…Through this process the magnetic energy is converted into plasma kinetic energy in bulk plasma flow, thermal and nonthermal particle distributions [1,2]. Reconnection plays a significant role in a wide range of laboratory, space, and astrophysical systems [3,4]. An important problem that remains unsolved is the acceleration of nonthermal charged particles in the reconnection region.…”

Section: Introductionmentioning

confidence: 99%

Particle acceleration during magnetic reconnection in a low-beta pair plasma

Guo

Daughton

et al. 2016

Physics of Plasmas

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Plasma energization through magnetic reconnection in the magnetically-dominated regime featured by low plasma beta (β = 8πnkT 0 /B 2 1) and/or high magnetizationis important in a series of astrophysical systems such as solar flares, pulsar wind nebula, and relativistic jets from black holes, etc. In this paper, we review the recent progress on kinetic simulations of this process and further discuss plasma dynamics and particle acceleration in a low-β reconnection layer that consists of electron-positron pairs. We also examine the effect of different initial thermal temperatures on the resulting particle energy spectra. While earlier papers have concluded that the spectral index is smaller for higher σ, our simulations show that the spectral index approaches p = 1 for sufficiently low plasma β, even if σ ∼ 1. Since this predicted spectral index in the idealized limit is harder than most observations, it is important to consider effects that can lead to a softer spectrum such as open boundary simulations. We also remark that the effects of 3D reconnection physics and turbulence on reconnection need to be addressed in the future.

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“…Theoretically, magnetic reconnection is extremely difficult to model (e.g., Yamada et al 2010;Zweibel & Yamada 2009). Models that have been made reveal the possibility of magnetic islands, accelerated particles, shocks, flows, and turbulence (e.g., Drake et al 2006;Hamilton & Petrosian 1992;Liu et al 2008).…”

Section: Introductionmentioning

confidence: 99%

Plasma Dynamics Above Solar Flare Soft X-Ray Loop Tops

Doschek

McKenzie

Warren

2014

ApJ

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We measure non-thermal motions in flare loop tops and above the loop tops using profiles of highly ionized spectral lines of Fe xxiv and Fe xxiii formed at multimillion-degree temperatures. Non-thermal motions that may be due to turbulence or multiple flow regions along the line of sight are extracted from the line profiles. The non-thermal motions are measured for four flares seen at or close to the solar limb. The profile data are obtained using the Extreme-ultraviolet Imaging Spectrometer on the Hinode spacecraft. The multimillion-degree non-thermal motions are between 20 and 60 km s −1 and appear to increase with height above the loop tops. Motions determined from coronal lines (i.e., lines formed at about 1.5 MK) tend to be smaller. The multimillion-degree temperatures in the loop tops and above range from about 11 MK to 15 MK and also tend to increase with height above the bright X-rayemitting loop tops. The non-thermal motions measured along the line of sight, as well as their apparent increase with height, are supported by Solar Dynamics Observatory Atmospheric Imaging Assembly measurements of turbulent velocities in the plane of the sky.

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Magnetic Reconnection in Astrophysical and Laboratory Plasmas

Cited by 530 publications

References 212 publications

Nonthermal particles and photons in starburst regions and superbubbles

Nonthermal particles and photons in starburst regions and superbubbles

Particle acceleration during magnetic reconnection in a low-beta pair plasma

Plasma Dynamics Above Solar Flare Soft X-Ray Loop Tops

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