Abstract
We report on a new method to compute the flare reconnection (RC) flux from post-eruption arcades (PEAs) and the underlying photospheric magnetic fields. In previous works, the RC flux has been computed using the cumulative flare ribbon area. Here we obtain the RC flux as the flux in half of the area underlying the PEA in EUV imaged after the flare maximum. We apply this method to a set of 21 eruptions that originated near the solar disk center in Solar Cycle 23. We find that the RC flux from the arcade method (\(\Phi_{\mathrm{rA}}\)) has excellent agreement with the flux from the flare-ribbon method (\(\Phi_{\mathrm{rR}}\)) according to \(\Phi_{\mathrm{rA}} = 1.24(\Phi_{\mathrm{rR}})^{0.99}\). We also find \(\Phi_{\mathrm{rA}}\) to be correlated with the poloidal flux (\(\Phi_{\mathrm{P}}\)) of the associated magnetic cloud at 1 AU: \(\Phi_{\mathrm{P}} = 1.20(\Phi_{\mathrm{rA}})^{0.85}\). This relation is nearly identical to that obtained by Qiu et al. (Astrophys. J. 659, 758, 2007) using a set of only 9 eruptions. Our result supports the idea that flare reconnection results in the formation of the flux rope and PEA as a common process.
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Acknowledgements
We thank the ACE, Wind and SOHO teams for providing the data on line. SOHO is a project of international collaboration between ESA and NASA. We thank C. Möstl for providing the poloidal flux of 13 magnetic clouds using the Grad–Shafranov method. Our work was supported by NASA’s Living with a Star Program.
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Earth-affecting Solar Transients
Guest Editors: Jie Zhang, Xochitl Blanco-Cano, Nariaki Nitta, and Nandita Srivastava
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Gopalswamy, N., Yashiro, S., Akiyama, S. et al. Estimation of Reconnection Flux Using Post-eruption Arcades and Its Relevance to Magnetic Clouds at 1 AU. Sol Phys 292, 65 (2017). https://doi.org/10.1007/s11207-017-1080-9
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DOI: https://doi.org/10.1007/s11207-017-1080-9