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Magnetic Reconnection in Solar Flares
Hvar Observatory bulletin, 2004Various aspects of solar flares are considered in the framework of analytic solutions of the complete set of MHD equations describing the the 2.5-D Petchek's reconnection model. In particular, we compare the theoretical results with characteristics of two-ribbon flares since they provide spatially resolved measurements of various plasma parameters.
Skender, Marina, Vršnak, Bojan
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Explosive events and magnetic reconnection in the solar atmosphere
AIP Conference Proceedings, 1992Explosive events are highly‐dynamic, small‐scale phenomena commonly observed in spectra of transition zone lines. Their velocities are near 100 km s−1, sizes near 1500 km, and time scales near 60 s. They occur at a height of 1000–2000 km, below typical transition zone structures.
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Analysis of Magnetic Reconnections and Compression of Magnetic Islands in the Solar Wind
Russian Journal of Mathematical Physics, 2018zbMATH Open Web Interface contents unavailable due to conflicting licenses.
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Solar Magnetic Topologies and Reconnection
2013A review is presented on the topology and eruption of twisted magnetic configurations in connection with eruptive flares, dynamical disparition brusque of prominences, and coronal mass ejections. A classical view of magnetic reconnection is mainly based on the MHD physics of 2-D configurations with an X-type neutral point, or on the extension of it to ...
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Role of magnetic reconnection in solar flares
Advances in Space Research, 1986Abstract The behaviour of the magnetic field in the solar atmosphere is governed by the equations of MHD rather than the electromagnetism of wires. In particular, the roles of magnetic reconnection are: to create small flares; to trigger large flares; and to release magnetic energy in large flares.
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Solar magnetic reconnection seen in detail
Physics Today, 2013New observations provide the most complete picture yet for the most energetic explosions in the solar system.
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Magnetic reconnection and some solar applications
Philosophical Transactions of the Royal Society of London. Series A: Mathematical, Physical and Engineering Sciences, 2000Magnetic reconnection is a fundamental plasma–physics process that is of great importance for the Sun, the Earth9s magnetosphere and all astrophysical objects which have magnetic fields. It is a process central to the generation of magnetic fields in stars and also plays a major role in the heating of solar and stellar coronae.
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The Criterion of Magnetic Reconnection in the Solar Wind
2015Ever since the “direct evidence” of magnetic reconnection in solar wind has been proposed by Gosling et al. (2005a), many reconnection exhausts are reported (Gosling et al. 2005a, b; Davis et al. 2006; Phan et al. 2006; Gosling et al. 2007a, b; Huttunen et al. 2007; Lavraud et al. 2009; Tian et al. 2010; Wang et al. 2010; Gosling 2011; Xu et al. 2011).
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Magnetic reconnection exhausts in the solar wind
2016The restructuring of magnetic fields in plasmas through the process of magnetic reconnection is important in laboratory experiments, magnetospheres and many astrophysical systems. In-situ observations of reconnection processes in the near-Earth environment provide an excellent opportunity to probe the physics of magnetic reconnection. In the solar wind,
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On the evolution of magnetic reconnection in the solar wind
Magnetic reconnection is a fundamental process in astrophysical plasma, as it enables the dissipation of energy at kinetic scales as well as large-scale reconfiguration of the magnetic topology. In the solar wind, its quantitative role in plasma dynamics and particle energization remains an open question that is starting to come into focus as more ...Naïs Fargette +8 more
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