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   https://doi.org/10.1007/s11214-025-01142-0  

   Liu, Yi-Hsin; Hesse, Michael; Genestreti, Kevin; Nakamura, Rumi; Burch, James_L; Cassak, Paul_A; Bessho, Naoki; Eastwood, Jonathan_P; Phan, Tai; Swisdak, Marc; et al (February 2025, Space Science Reviews)

   Abstract Magnetic reconnection is a ubiquitous plasma process that transforms magnetic energy into particle energy during eruptive events throughout the universe. Reconnection not only converts energy during solar flares and geomagnetic substorms that drive space weather near Earth, but it may also play critical roles in the high energy emissions from the magnetospheres of neutron stars and black holes. In this review article, we focus on collisionless plasmas that are most relevant to reconnection in many space and astrophysical plasmas. Guided by first-principles kinetic simulations and spaceborne in-situ observations, we highlight the most recent progress in understanding this fundamental plasma process. We start by discussing the non-ideal electric field in the generalized Ohm’s law that breaks the frozen-in flux condition in ideal magnetohydrodynamics and allows magnetic reconnection to occur. We point out that this same reconnection electric field also plays an important role in sustaining the current and pressure in the current sheet and then discuss the determination of its magnitude (i.e., the reconnection rate), based on force balance and energy conservation. This approach to determining the reconnection rate is applied to kinetic current sheets with a wide variety of magnetic geometries, parameters, and background conditions. We also briefly review the key diagnostics and modeling of energy conversion around the reconnection diffusion region, seeking insights from recently developed theories. Finally, future prospects and open questions are discussed. 

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2. Relativistic Asymmetric Magnetic Reconnection

   https://doi.org/10.1103/PhysRevLett.128.145101  

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3. The reversibility of magnetic reconnection

   https://doi.org/10.1063/5.0050575  

   Xuan, M.; Swisdak, M.; Drake, J. F. (September 2021, Physics of Plasmas)

   null (Ed.)
4. Nonlinear Reconnection in Magnetized Turbulence

   https://doi.org/10.3847/1538-4357/ab6a95  

   Loureiro, Nuno F.; Boldyrev, Stanislav (February 2020, The Astrophysical Journal)
5. Dimensionality of solar magnetic reconnection

   https://doi.org/10.1007/s41614-022-00096-y  

   Lee, Jeongwoo (December 2022, Reviews of Modern Plasma Physics)

   Abstract Solar flares are the best examples of astrophysical magnetic reconnection in which the reconnection structure can be studied in detail. The structure is manifested through flare ribbons, intense optical and EUV emissions in footpoints of field lines attached to the coronal reconnection region. In the most common type of solar flares, two parallel ribbons appear and move away from each other, which could be related to the reconnection electric field under the theory of two-dimensional (2D) X-point reconnection, opening up a wide field of solar research. Another breakthrough came upon the discovery of circular ribbons, which implies a dome-shaped spine-fan structure capable of truly three dimensional (3D) null point reconnection. The variability of circular ribbons could also shed light on the reconnection electric field in the corona, but was relatively less attended. In this paper, we review selective topics in both types of flares with emphasis on the dimensionality of magnetic reconnection. Three types of reconnection: 2D X-point, 3D torsional, and 3D spine-fan reconnection are studied and associated with translational, rotational, and vibrational degrees of freedom. It is demonstrated that the dimensionality-based analysis of the observed dynamics of circular and parallel ribbons can facilitate a better understanding of the nature of solar magnetic reconnection. 

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