Magnetic helicity change rate associated with three x-class eruptive flares

Document Type

Article

Publication Date

1-1-2003

Abstract

In this paper we have examined the temporal evolution of magnetic helicity change rate associated with three X-class eruptive flares that occured on November 24, 2000. By analyzing a set of 1 minute cadence high-resolution magnetograms taken by Michelson Doppler Imager (MDI) on board Solar and Heliospheric Observatory (SOHO), we have determined the rates of magnetic helicity transport via horizontal photospheric motions. Then we have compared the impulsive variations of helicity injection rate with an initial eruption speed profile of a filament associated with a X1.8 flare. As a result, we have found (1) that the impulsive variations of magnetic helicity change rate were strongly correlated with only three X-class flarings, (2) that the eruption of the filament started about 10 minutes before the impulsive variation of the helicity change rate, and (3) that horizontal velocity kernels were located between Hα two flaring ribbons. Thus we suggest that the observed impulsive helicity change is not a cause of the eruptive solar flare but its result, i.e., photospheric response to the coronal field restructuring. © 2003 COSPAR. Published by Elsevier Ltd. All rights reserved.

Identifier

0345790410 (Scopus)

Publication Title

Advances in Space Research

External Full Text Location

https://doi.org/10.1016/S0273-1177(03)90632-6

ISSN

02731177

First Page

1953

Last Page

1958

Issue

10

Volume

32

Grant

INT-98-16267

Fund Ref

National Science Foundation

This document is currently not available here.

Share

COinS