A statistical study of energy release and transport midway between the magnetic reconnection and initial dipolarization regions in the near-Earth magnetotail associated with substorm expansion onsets

2012 ◽  
Vol 117 (A11) ◽  
pp. n/a-n/a ◽  
Author(s):  
Y. Miyashita ◽  
S. Machida ◽  
M. Nosé ◽  
K. Liou ◽  
Y. Saito ◽  
...  
Keyword(s):  
Magnetic Reconnection ◽  
Energy Release ◽  
Statistical Study

Magnetic reconnection and energy release in a long-duration stellar flare

1986 ◽  
Vol 6 (8) ◽  
pp. 145-148 ◽  
Author(s):  
G. Poletto ◽  
R. Pallavicini ◽  
R.A. Kopp
Keyword(s):  
Magnetic Reconnection ◽  
Energy Release ◽  
Stellar Flare ◽  
Long Duration

Possible two-step solar energy release mechanism due to turbulent magnetic reconnection

2005 ◽  
Vol 12 (5) ◽  
pp. 052901 ◽  
Author(s):  
Quan-Lin Fan ◽  
Xue-Shang Feng ◽  
Chang-Qing Xiang
Keyword(s):  
Solar Energy ◽  
Magnetic Reconnection ◽  
Energy Release ◽  
Release Mechanism

scholarly journals Hard X-ray Spectrum of the Above-the-Looptop Source in Impulsive Solar Flares

2000 ◽  
Vol 195 ◽  
pp. 413-414
Author(s):  
S. Masuda
Keyword(s):  
Magnetic Reconnection ◽  
Energy Release ◽  
Solar Flares ◽  
Count Rate ◽  
High Quality ◽  
X Ray ◽  
Flare Energy

Extended AbstractThe Hard X-ray Telescope (HXT: Kosugi et al. 1991) onboard Yohkoh has observed that, in impulsive solar flares, a hard X-ray source is located above the apex of a soft X-ray flaring loop, in addition to double footpoint sources (Masuda et al. 1994, 1995). This observation suggests that flare energy-release, probably magnetic reconnection, takes place not in the soft X-ray loop but above the loop. It is important to derive the hard X-ray spectrum of the above-the-looptop source accurately in order to understand how electrons are energized there. The above-the-looptop source was most clearly observed during the 13 January 1992 flare. However, the count rate, especially in the H-band (53–93 keV), is too small to synthesize high-quality images and to derive an accurate spectrum.

scholarly journals The role of compressibility in energy release by magnetic reconnection

2012 ◽  
Vol 19 (8) ◽  
pp. 082109 ◽  
Author(s):  
J. Birn ◽  
J. E. Borovsky ◽  
M. Hesse
Keyword(s):  
Magnetic Reconnection ◽  
Energy Release

scholarly journals A statistical study of fast magnetic reconnection in turbulent accretion disks and jets

2019 ◽  
Author(s):  
Luis H.S. Kadowaki ◽  
Elisabete De Gouveia Dal Pino ◽  
Tania E. Medina-Torrejon
Keyword(s):  
Magnetic Reconnection ◽  
Accretion Disks ◽  
Statistical Study

Coronal Heating: Energy Release Associated with Chromospheric Magnetic Reconnection

2000 ◽  
Vol 538 (2) ◽  
pp. 960-967 ◽  
Author(s):  
Colin B. Roald ◽  
P. A. Sturrock ◽  
Richard Wolfson
Keyword(s):  
Magnetic Reconnection ◽  
Energy Release ◽  
Coronal Heating

scholarly journals Magnetic reconnection and energy release on the Sun and solar-like stars

2008 ◽  
Vol 4 (S259) ◽  
pp. 191-200
Author(s):  
Lidia van Driel-Gesztelyi
Keyword(s):  
Free Energy ◽  
Magnetic Reconnection ◽  
Energy Release ◽  
Energy Content ◽  
Magnetic Flux Density ◽  
The Sun ◽  
X Rays ◽  
Stellar Flares ◽  
Wide Wavelength Range ◽  
Hot Corona

AbstractMagnetic reconnection is thought to play an important role in liberating free energy stored in stressed magnetic fields. The consequences vary from undetectable nanoflares to huge flares, which have signatures over a wide wavelength range, depending on e.g. magnetic topology, free energy content, total flux, and magnetic flux density of the structures involved. Events of small energy release, which are thought to be the most numerous, are one of the key factors in the existence of a hot corona in the Sun and solar-like stars. The majority of large flares are ejective, i.e. involve the expulsion of large quantities of mass and magnetic field from the star. Since magnetic reconnection requires small length-scales, which are well below the spatial resolution limits of even the solar observations, we cannot directly observe magnetic reconnection happening. However, there is a plethora of indirect evidences from X-rays to radio observations of magnetic reconnection. I discuss key observational signatures of flares on the Sun and solar-paradigm stellar flares and describe models emphasizing synergy between observations and theory.

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