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

Statistical properties of X-class flares and their relationship with super active regions during solar cycles 21–23

2014 ◽  
Vol 350 (2) ◽  
pp. 443-447 ◽  
Author(s):  
Guiming Le ◽  
Xingxing Yang ◽  
Yonghua Liu ◽  
Peng Li ◽  
Zhiqiang Yin ◽  
...  
Keyword(s):  
Active Regions ◽  
Statistical Properties ◽  
Solar Cycles

Statistical Properties of Magnetic Separators in Model Active Regions

1999 ◽  
Vol 522 (2) ◽  
pp. 1117-1132 ◽  
Author(s):  
Brian T. Welsch ◽  
Dana W. Longcope
Keyword(s):  
Active Regions ◽  
Statistical Properties

STATISTICAL PROPERTIES OF SOLAR FLARES AND COMPARISON TO OTHER IMPULSIVE ENERGY RELEASE EVENTS

2009 ◽  
Vol 23 (28n29) ◽  
pp. 5609-5618 ◽  
Author(s):  
FABIO LEPRETI ◽  
VLADIMIR G. KOSSOBOKOV ◽  
VINCENZO CARBONE
Keyword(s):  
Solar Flare ◽  
Energy Release ◽  
Solar Flares ◽  
Statistical Properties ◽  
Universal Curve ◽  
Mhd Turbulence ◽  
Natural Systems ◽  
Self Organized ◽  
Self Organized Criticality ◽  
Impulsive Processes

Impulsive energy release events are observed in many natural systems. Solar flares are certainly among the most remarkable examples of such processes. In the last years the study of solar flare statistical properties has received considerable attention in the context of solar flare models based on different approaches, such as Self Organized Criticality (SOC) or magnetohydrodynamic (MHD) turbulence. In this talk the main statistical properties of solar flares will be presented and compared to those of other well known impulsive processes, such as earthquakes and soft γ-ray flashes occurring on neutron stars. It is shown that the these phenomena are characterized by different statistics that cannot be rescaled onto a single, universal curve and that this holds even for the same phenomenon, when observed in different periods or at different locations. Our results indicate apparent complexity of impulsive energy release processes, which neither follow a common behavior nor could be attributed to a universal physical mechanism.

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 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.

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