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Magnetic structure of solar flare regions producing hard X-ray pulsations
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Zimovets, I. V., Wang, R., Liu, Y. D., Wang, C., Kuznetsov, S. A., Sharykin, I. N., Struminsky, A. B. and Nakariakov, V. M. (Valery M.) (2018) Magnetic structure of solar flare regions producing hard X-ray pulsations. Journal of Atmospheric and Solar-Terrestrial Physics, 174 . pp. 17-27. doi:10.1016/j.jastp.2018.04.017 ISSN 1364-6826.
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WRAP-magnetic-structure-solar-flare-regions-hard-pulsations-Nakariakov-2018.pdf - Accepted Version - Requires a PDF viewer. Available under License Creative Commons Attribution Non-commercial No Derivatives 4.0. Download (644Kb) | Preview |
Official URL: https://doi.org/10.1016/j.jastp.2018.04.017
Abstract
We present analysis of the magnetic field in seven solar flare regions accompanied by the pulsations of hard X-ray (HXR) emission. These flares were studied by Kuznetsov et al. (2016) (Paper I), and chosen here because of the availability of the vector magnetograms for their parent active regions (ARs) obtained with the SDO/HMI data. In Paper I, based on the observations only, it was suggested that a magnetic flux rope (MFR) might play an important role in the process of generation of the HXR pulsations. The goal of the present paper is to test this hypothesis by using the extrapolation of magnetic field with the non-linear force-free field (NLFFF) method. Having done this, we found that before each flare indeed there was an MFR elongated along and above a magnetic polarity inversion line (MPIL) on the photosphere. In two flare regions the sources of the HXR pulsations were located at the footpoints of different magnetic field lines wrapping around the central axis, and constituting an MFR by themselves. In five other flares the parent field lines of the HXR pulsations were not a part of an MFR, but surrounded it in the form of an arcade of magnetic loops. These results show that, at least in the analyzed cases, the “single flare loop” models do not satisfy the observations and magnetic field modeling, while are consistent with the concept that the HXR pulsations are a consequence of successive episodes of energy release and electron acceleration in different magnetic flux tubes (loops) of a complex AR. An MFR could generate HXR pulsations by triggering episodes of magnetic reconnection in different loops in the course of its non-uniform evolution along an MPIL. However, since three events studied here were confined flares, actual eruptions may not be required to trigger sequential particle acceleration episodes in the magnetic systems containing an MFR.
| Item Type: | Journal Article | |||||||||||||||||||||
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| Subjects: | Q Science > QB Astronomy | |||||||||||||||||||||
| Divisions: | Faculty of Science, Engineering and Medicine > Science > Physics | |||||||||||||||||||||
| SWORD Depositor: | Library Publications Router | |||||||||||||||||||||
| Library of Congress Subject Headings (LCSH): | Solar flares -- Magnetic fields, Solar photosphere | |||||||||||||||||||||
| Journal or Publication Title: | Journal of Atmospheric and Solar-Terrestrial Physics | |||||||||||||||||||||
| Publisher: | Elsevier BV | |||||||||||||||||||||
| ISSN: | 1364-6826 | |||||||||||||||||||||
| Official Date: | September 2018 | |||||||||||||||||||||
| Dates: |
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| Volume: | 174 | |||||||||||||||||||||
| Page Range: | pp. 17-27 | |||||||||||||||||||||
| DOI: | 10.1016/j.jastp.2018.04.017 | |||||||||||||||||||||
| Status: | Peer Reviewed | |||||||||||||||||||||
| Publication Status: | Published | |||||||||||||||||||||
| Access rights to Published version: | Restricted or Subscription Access | |||||||||||||||||||||
| Date of first compliant deposit: | 8 August 2018 | |||||||||||||||||||||
| Date of first compliant Open Access: | 1 May 2019 | |||||||||||||||||||||
| RIOXX Funder/Project Grant: |
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