Mathematics – Logic
Scientific paper
May 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agusmsp43a..08k&link_type=abstract
American Geophysical Union, Spring Meeting 2008, abstract #SP43A-08
Mathematics
Logic
2723 Magnetic Reconnection (7526, 7835), 7519 Flares, 7526 Magnetic Reconnection (2723, 7835), 7835 Magnetic Reconnection (2723, 7526)
Scientific paper
In this work we study an eruptive flare event in order to quantitatively understand flux and helicity transfer through reconnection in the associated coronal flux rope formation. Quantitative observational studies of solar flare reconnection have been made by a number of research groups (Poletto and Kopp, 1986, Fletcher and Hudson 2001, Qiu and Yurchyshyn, 2005). However, their work does not allow one to predict, from observations, both the flux and twist that coronal reconnection contributes to interplanetary flux ropes. Our hypothesis is that the flux and helicity associated with eruptive solar flares is created through a sequence of magnetic reconnections. Longcope et al. (2007) introduced a topological method of studying flux rope formation in 3D. In our study we use MDI, SOHO and TRACE data. We apply two methods to derive the reconnection sequence: (1) the flaring sequence from the TRACE observations of ribbon brightening (Qiu et al, 2007) and (2) the reconnection sequence from the topological model of the coronal field based on the Minimum Current Corona model (Longcope, 2001). From the topological model we calculate the toroidal flux and total helicity of the flux rope. We study in detail the M8.0 flare in active region NOAA 10759, 13-May-2005 16:13UT. The total magnetic flux of the active region is 1.7 ·10 22 Mx. From the photospheric magnetogram evolution we determine that 1.9 · 1042 Mx2 of magnetic helicity has been injected into the active region during the 40-hour build-up prior to the flare. From the domain flux evolution we show that reconnection in the model (2) must occur in a specific sequence which would produce a twisted flux rope containing significantly less flux and helicity than the whole active region. The reconnection sequence from the model (2) compares favorably with the one inferred from the observation sequence (1). However, the topological analysis might be sensitive to the beginning of the buildup time, so its choice will be discussed.
Canfield Richard C.
Kazachenko Maria
Longcope Dana Warfield
Qiu Jianwei
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