Results 231 to 240 of about 23,617 (267)

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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Magnetic Reconnection in the Solar Wind

Space Science Reviews, 2011
It is only within the last 5 years that we have learned how to recognize the unambiguous signature of magnetic reconnection in the solar wind in the form of roughly Alfvenic accelerated plasma flows embedded within bifurcated magnetic field reversal regions (current sheets).
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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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Magnetic Reconnection in the Solar Lower Atmosphere

2002
ABSTRACT There are many active phenomena, such as Ellerman bombs (EBs), Type II white-light flares (WLFs) etc, appear in the solar lower atmosphere. They have many common features despite of the large energy gap between them. They are considered to result from the local heating in the solar lower atmosphere.
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Magnetic reconnection in solar eruptive events of varying magnetic configurations

Journal of Atmospheric and Solar-Terrestrial Physics, 2007
We study the relationship between magnetic reconnection and acceleration of filaments and coronal mass ejections (CMEs) in different magnetic configurations. They occur in either quiet-Sun or active regions of either bipolar or multipolar magnetic fields, and are either or not accompanied by filament eruptions.
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Evidence of Magnetic Reconnection in Solar Flares

1996
The detailed analysis of the 1992 February 21 flare indicates that magnetic reconnection is responsible for heating of the thermal plasmas produced in the flare. The plasma density enhancement presumably associated with slow shocks is observed. The Yohkoh observations of this flare fit well with the Petschek model, and the structure of the slow shock ...
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