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Magnetic Reconnection Flux during Two Flares on September 6, 2017

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Abstract

We analyzed the dynamics of the reconnection and energy release processes of the X2.2 and X9.3 flares that occurred on September 6, 2017 in the active region NOAA 12673. We used SDO/AIA 1600 Å images together with SDO/HMI magnetograms. As a proxy for the flare energy release rate, we used the KRIM and RSTN microwave time profiles, GOES soft X-rays and its time derivative. Assuming that the chromospheric flare ribbons are located at the footpoints of magnetic field lines reconnecting in the corona and that the magnetic flux is conserved from the photosphere to the corona, we obtained magnetic reconnection fluxes and rates of its change. The cumulative positive and negative magnetic fluxes involved in the reconnection process were balanced. Temporal correlations are found between the calculated reconnection rate and the observed microwave emissions from for both events. An analysis of the total cumulative magnetic flux and SXR fluence of events showed that the magnitude of the magnetic flux involved in the reconnection process was greater in more energetic events and less in weaker ones.

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ACKNOWLEDGMENTS

SDO is a project of the NASA Living with a Star program. SDO/AIA and SDO/HMI data were provided by the Joint Science Operation Center (JSOC).

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This work was supported by ongoing institutional funding. No additional grants to carry out or direct thisparticular research were obtained.

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Authors and Affiliations

  1. Crimean Astrophysical Observatory, Russian Academy of Sciences, Republic of Crimea, Russia

    O. S. Gopasyuk, A. E. Volvach & I. V. Yakubovskaya

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  1. O. S. Gopasyuk
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  2. A. E. Volvach
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  3. I. V. Yakubovskaya
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Correspondence to O. S. Gopasyuk.

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Gopasyuk, O.S., Volvach, A.E. & Yakubovskaya, I.V. Magnetic Reconnection Flux during Two Flares on September 6, 2017. Geomagn. Aeron. 63, 1000–1006 (2023). https://doi.org/10.1134/S0016793223070095

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