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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

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Official URL: https://doi.org/10.1016/j.jastp.2018.04.017

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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
Subjects: Q Science > QB Astronomy
Divisions: Faculty of 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:
DateEvent
September 2018Published
1 May 2018Available
28 April 2018Accepted
Date of first compliant deposit: 8 August 2018
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
RIOXX Funder/Project Grant:
Project/Grant IDRIOXX Funder NameFunder ID
77352569British Councilhttp://dx.doi.org/10.13039/501100000308
15-02-0828[RFBR] Russian Foundation for Basic Researchhttp://dx.doi.org/10.13039/501100002261
16-32-50117[RFBR] Russian Foundation for Basic Researchhttp://dx.doi.org/10.13039/501100002261
16-02-00328[RFBR] Russian Foundation for Basic Researchhttp://dx.doi.org/10.13039/501100002261
16-12-10448[RSF] Russian Science Foundationhttp://dx.doi.org/10.13039/501100006769
1731070[NSFC] National Natural Science Foundation of Chinahttp://dx.doi.org/10.13039/501100001809

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