TY - JOUR
T1 - Magnetic helicity change rate associated with three x-class eruptive flares
AU - Moon, Y. J.
AU - Chae, Jongchul
AU - Wang, Haimin
AU - Park, Y. D.
N1 - Funding Information:
We are thankful to the BBS0 observing staff for obtaining the data. We appreciate the valuable comments of Dr. G. S. Choe, the editor, Dr. A. Pevtsov, and the referee. This work has been supported by NASA grants NAG5-10894 and NAG5-7837, by MURI grant of AFOSR, by the US-Korea Cooperative Science Program (NSF INT-98-16267), and by NRL M10104000059-01J000002500 of the Korean government.
PY - 2003
Y1 - 2003
N2 - 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.
AB - 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.
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U2 - 10.1016/S0273-1177(03)90632-6
DO - 10.1016/S0273-1177(03)90632-6
M3 - Article
AN - SCOPUS:0345790410
SN - 0273-1177
VL - 32
SP - 1953
EP - 1958
JO - Advances in Space Research
JF - Advances in Space Research
IS - 10
ER -