Energy release processes in active regions

2008 ◽  
pp. 201-217 ◽  
Author(s):  
Arnold O. Benz
Keyword(s):  
Energy Release ◽  
Active Regions ◽  
Release Processes

Two Energy-release Processes Observed in the Eruption of a Confined Filament System

2018 ◽  
Vol 130 (994) ◽  
pp. 124401 ◽  
Author(s):  
Hongbo Li ◽  
Yu Liu ◽  
Jihong Liu ◽  
A. Elmhamdi ◽  
A.-S. Kordi
Keyword(s):  
Energy Release ◽  
Filament System ◽  
Release Processes

scholarly journals About the nature of long-term microflare energy release in solar active regions

2001 ◽  
Vol 106 (A11) ◽  
pp. 25353-25360 ◽  
Author(s):  
Vladimir M. Bogod ◽  
Claude Mercier ◽  
Leonid V. Yasnov
Keyword(s):  
Energy Release ◽  
Active Regions ◽  
Solar Active Regions

On the periodicity of energy release in solar active regions

2005 ◽  
Vol 31 (6) ◽  
pp. 414-421 ◽  
Author(s):  
T. B. Goldvarg ◽  
Yu. A. Nagovitsyn ◽  
A. A. Solov’ev
Keyword(s):  
Energy Release ◽  
Active Regions ◽  
Solar Active Regions

scholarly journals Two energy release processes for CMEs: MHD catastrophe and magnetic reconnection

2007 ◽  
Vol 40 (12) ◽  
pp. 1780-1786 ◽  
Author(s):  
Y. Chen ◽  
Y.Q. Hu ◽  
L.D. Xia
Keyword(s):  
Magnetic Reconnection ◽  
Energy Release ◽  
Release Processes

scholarly journals Statistical Properties of the Energy Release in Emerging and Evolving Active Regions

2002 ◽  
Vol 575 (2) ◽  
pp. L87-L90 ◽  
Author(s):  
Loukas Vlahos ◽  
Tassos Fragos ◽  
Heinz Isliker ◽  
Manolis Georgoulis
Keyword(s):  
Energy Release ◽  
Active Regions ◽  
Statistical Properties

scholarly journals Nanoflares and the Heating of the Solar Corona

2004 ◽  
Vol 219 ◽  
pp. 461-472
Author(s):  
Arnold O. Benz
Keyword(s):  
Energy Source ◽  
Solar Wind ◽  
Energy Release ◽  
Active Regions ◽  
Heating Process ◽  
Back Reaction ◽  
The Sun ◽  
Line Broadening ◽  
Higher Temperature ◽  
The Impact

New observational signatures of the heating process(es) have been revealed by space missions including SoHO, TRACE, Yohkoh, and RHESSI. Evidences for heating in the quiet corona, active region loops, and the solar wind are different and must be distinguished. Prime indications come from line broadening and waves, the distribution of temperature and radiation loss in relation to height, the correlation of magnetic flux and brightness, nanoflares and other fluctuations. This review concentrates on microevents observed at coronal temperatures. The reported nanoflares in quiet regions are about 2 orders of magnitude smaller than microflares reported in active regions and exhibit less radio emission. To estimate the impact of these microevents on the corona, the effects from a localized energy release must be considered, regardless of the energy source (reconnection or waves). In particular, the coupling with the chromosphere, i.e. the back-reaction of the chromosphere on coronal energy release, has an important effect on the corona. A necessary requirement for the heating process(es) is to deposit most of the heat in the low corona, but to heat also the upper corona to even higher temperature. Finally, the heating process must be able to account for the coronae of more active stars showing coronal emissions at levels of more than 3 orders of magnitude higher than the Sun.

Observational Tests of a Double Loop Model for Solar Flares

1998 ◽  
Vol 15 (3) ◽  
pp. 318-324 ◽  
Author(s):  
S. J. Hardy ◽  
D. B. Melrose ◽  
H. S. Hudson
Keyword(s):  
Magnetic Reconnection ◽  
Energy Release ◽  
Numerical Investigation ◽  
Solar Flares ◽  
Active Regions ◽  
Double Loop ◽  
Loop Model ◽  
Strong Relation

AbstractA model for the energetics of solar flares, developed by Melrose (1997), is based on magnetic reconnection between two current-carrying magnetic loops. A detailed numerical investigation of the model has been made to identify those configurations that lead to energy release in a flare. Our results predict a strong relation between the ratio of currents in the interacting loops for a favoured flare configuration, and provide further support for a proposed method of generating long loops connecting different active regions. Both of these predictions are amenable to observational verification.

Collaborative VLA, SOHO and RHESSI observations of evolving sources of energy release in the corona above active regions

2005 ◽  
Vol 35 (10) ◽  
pp. 1813-1821 ◽  
Author(s):  
Robert F. Willson
Keyword(s):  
Energy Release ◽  
Active Regions

Synoptic Charts of the Solar Eclipses of 1990 and 1991

1994 ◽  
Vol 144 ◽  
pp. 517-521
Author(s):  
Z. Mouradian ◽  
G. Buchholtz ◽  
G. Zlicaric
Keyword(s):  
Solar Limb ◽  
Active Regions ◽  
Solar Eclipses ◽  
Coronal Structures

AbstractThe synoptic charts of solar rotations 1831 and 1844 have been drawn up, corresponding to the eclipses of 22 July 1990 and 11 July 1991. These charts contain the active regions and the filaments, and show the position of the solar limb, at the time of the eclipse. They are for use in studying the coronal structures observed during these eclipses. The variation of these structures is given in the table. The last section of the article contains a formula for identifying the structures out of the limb.

Solar Corona Investigation by the Coronal Line Photometer at Lomnický Peak

1994 ◽  
Vol 144 ◽  
pp. 431-434
Author(s):  
M. Minarovjech ◽  
M. Rybanský
Keyword(s):  
Solar Corona ◽  
Time Resolution ◽  
Active Regions ◽  
High Time ◽  
High Time Resolution ◽  
List Type ◽  
Type Number ◽  
Coronal Line ◽  
Global Cycle

AbstractThis paper deals with a possibility to use the ground-based method of observation in order to solve basic problems connected with the solar corona research. Namely:1.heating of the solar corona2.course of the global cycle in the corona3.rotation of the solar corona and development of active regions.There is stressed a possibility of high-time resolution of the coronal line photometer at Lomnický Peak coronal station, and use of the latter to obtain crucial observations.

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