Flux emergence, flux imbalance, magnetic free energy and solar flares

被引：20

作者：

Choudhary, Debi Prasad ^{[1
]}

Gosain, Sanjay ^{[2
]}

Gopalswamy, Nat ^{[3
]}

Manoharan, P. K. ^{[7
]}

Chandra, R. ^{[6
]}

Uddin, W. ^{[5
]}

Srivastava, A. K. ^{[5
]}

Yashiro, S. ^{[3
]}

Joshi, N. C. ^{[5
]}

Kayshap, P. ^{[5
]}

Dwivedi, V. C. ^{[7
]}

Mahalakshmi, K. ^{[7
]}

Elamathi, E. ^{[7
]}

Norris, Max ^{[1
]}

Awasthi, A. K. ^{[4
]}

Jain, R. ^{[4
]}

机构：

[1] Calif State Univ Northridge, Dept Phys & Astron, Northridge, CA 91330 USA

[2] Natl Opt Astron Observ, Natl Solar Observ, Tucson, AZ 85726 USA

[3] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA

[4] Phys Res Lab, Dept Space, Ahmadabad 380009, Gujarat, India

[5] Aryabhatta Res Inst Observat Sci ARIES, Naini Tal 263129, India

[6] Kumaun Univ, Dept Phys, Naini Tal 263002, India

[7] Tata Inst Fundamental Res, NCRA, Radio Astron Ctr, Udhagamandalam Ooty 643001, India

来源：

ADVANCES IN SPACE RESEARCH | 2013年 / 52卷 / 08期

关键词：

Flux emergence; Flux imbalance; Magnetic free energy; Sunspot area; Solar flare; CORONAL MASS EJECTION; EMERGING FLUX; FIELD; INTENSITY; REGIONS; SUN;

D O I：

10.1016/j.asr.2013.07.009

中图分类号：

V [航空、航天];

学科分类号：

08 ; 0825 ;

摘要：

Emergence of complex magnetic flux in the solar active regions lead to several observational effects such as a change in sunspot area and flux embalance in photospheric magnetograms. The flux emergence also results in twisted magnetic field lines that add to free energy content. The magnetic field configuration of these active regions relax to near potential-field configuration after energy release through solar flares and coronal mass ejections. In this paper, we study the relation of flare productivity of active regions with their evolution of magnetic flux emergence, flux imbalance and free energy content. We use the sunspot area and number for flux emergence study as they contain most of the concentrated magnetic flux in the active region. The magnetic flux imbalance and the free energy are estimated using the HMI/SDO magnetograms and Virial theorem method. We find that the active regions that undergo large changes in sunspot area are most flare productive. The active regions become flary when the free energy content exceeds 50% of the total energy. Although, the flary active regions show magnetic flux imbalance, it is hard to predict flare activity based on this parameter alone. (C) 2013 COSPAR. Published by Elsevier Ltd. All rights reserved.

引用

页码：1561 / 1566

页数：6

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