HR: 16:00h
AN: SP44A-03    [Abstracts]
TI: On the Relationship Among Magnetic Twist, Reconnection Rate and Acceleation in Solar Eruptions
AU: * Jing, J
EM: jj4@njit.edu
AF: Big Bear Solar Observatory New Jersey Institute of Tech., Center for Solar and Terrestrial Research Unversity Height, Newark, NJ 07102
AU: Yurchyshyn, V
EM: vayur@bbso.njit.edu
AF: Big Bear Solar Observatory New Jersey Institute of Tech., Center for Solar and Terrestrial Research Unversity Height, Newark, NJ 07102
AU: Qiu, J
EM: qiuj@bbso.njit.edu
AF: Big Bear Solar Observatory New Jersey Institute of Tech., Center for Solar and Terrestrial Research Unversity Height, Newark, NJ 07102
AU: Xu, Y
EM: yx2@njit.edu
AF: Big Bear Solar Observatory New Jersey Institute of Tech., Center for Solar and Terrestrial Research Unversity Height, Newark, NJ 07102
AU: Wang, H
EM: haimin@flare.njit.edu
AF: Big Bear Solar Observatory New Jersey Institute of Tech., Center for Solar and Terrestrial Research Unversity Height, Newark, NJ 07102
AB: We investigate the statistical correlation between the magnetic twist and properties of solar eruptions such as acceleration of eruptive filaments and magnetic reconnection rate of corresponding two-ribbon flares. We anticipate to provide observational evidence for, or against, the speculation that increasing magnetic twist is more likely giving rise to the violent solar eruptions. The magnetic twist is characterized by the linear force-free (LFFF) magnetic field constant α. We adopt a method for the reconstruction of the LFFF magnetic field in a bounded domain that was described in Abramenko and Yurchishin (1996). The best-fit value of α is selected so that the extrapolated field gives the closest match to the coronal observations. The magnetic reconnection rate of two-ribbon flares, in terms of electric field inside the reconnecting current sheet(RCS) and flux change rate involved in magnetic reconnection in the low corona, is derived by measuring the expansion of flare ribbons across the the magnetic field. Based our limited events studied so far, there appears to be a tendency that the magnetic field with higher α shows higher filament acceleration and magnetic reconnection rate.
DE: 7513 Coronal mass ejections
DE: 7519 Flares
DE: 7524 Magnetic fields
DE: 7531 Prominence eruptions
SC: Solar Physics Division - AAS [SP]
MN: 2005 Joint Assembly