Results 181 to 190 of about 23,056 (219)

Magnetic reconnection in solar flares

Geophysical & Astrophysical Fluid Dynamics, 1991
The magnetic energy stored in the corona is the only plausible source for the energy released during large solar flares. During the last 20 years most theoretical work has concentrated on models which store magnetic energy in the corona in the form of electrical currents, and a major goal of present day research is to understand how these currents are ...
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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, 2000
Magnetic 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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Solar magnetic reconnection seen in detail

Physics Today, 2013
New observations provide the most complete picture yet for the most energetic explosions in the solar system.
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Solar Flares and Magnetic Reconnection

2005
Abstract Recent studies by the author and his colleagues on solar flares based on the magnetic reconnection model are reviewed. The studies have been done mainly by using the data sets of space-craft observations and super-computer simulations. The covered topics are an EUV observation of reconnection inflows, MHD simulations of the reconnection ...
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Magnetic Reconnection in Solar Flares

Hvar Observatory bulletin, 2004
Various 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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Solar Magnetic Topologies and Reconnection

2013
A 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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Magnetic Reconnection in the Solar Wind: An Update

AIP Conference Proceedings, 2010
Magnetic reconnection in the solar wind commonly occurs in a quasi‐stationary mode. It produces extensive Petschek‐like exhausts of roughly Alfvenic jetting plasma typically bounded by back‐to‐back rotational discontinuities that bifurcate a reconnecting current sheet. It occurs most frequently at current sheets associated with relatively small (
J. T. Gosling, M. Maksimovic, K. Issautier, N. Meyer-Vernet, M. Moncuquet, F. Pantellini   +5 more
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Role of magnetic reconnection in solar flares

Advances in Space Research, 1986
Abstract 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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Direct indication of magnetic reconnection in solar photosphere

Chinese Astronomy and Astrophysics, 1992
Abstract A direct indication of magnetic reconnection in solar photosphere has been found for the first time with the aid of the time sequence of vector magnetograms. The reconnection takes place in the interface between one pole of an emerging flux region and the old flux of opposite polarity.
null Wang Jing-xiu, null Shi Zhong-xian
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Explosive events and magnetic reconnection in the solar atmosphere

AIP Conference Proceedings, 1992
Explosive 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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