Issue |
A&A
Volume 683, March 2024
|
|
---|---|---|
Article Number | A87 | |
Number of page(s) | 16 | |
Section | The Sun and the Heliosphere | |
DOI | https://doi.org/10.1051/0004-6361/202348275 | |
Published online | 08 March 2024 |
Using relative field line helicity as an indicator for solar eruptivity
1
Physics Department, University of Ioannina, Ioannina 45110, Greece
e-mail: k.moraitis@uoi.gr
2
University of Graz, Institute of Physics/IGAM, Graz, Austria
3
Sorbonne Université, École polytechnique, Institut Polytechnique de Paris, Université Paris-Saclay, Observatoire de Paris-PSL, CNRS, Laboratoire de Physique des Plasmas (LPP), 4 place Jussieu, 75005 Paris, France
Received:
13
October
2023
Accepted:
20
December
2023
Context. Relative field line helicity (RFLH) is a recently developed quantity that can approximate the density of relative magnetic helicity.
Aims. This paper aims to determine whether RFLH can be used as an indicator of solar eruptivity.
Methods. Starting from magnetographic observations from the Helioseismic and Magnetic Imager instrument on board the Solar Dynamic Observatory of a sample of seven solar active regions (ARs), that comprises over 2000 individual snapshots, we reconstruct the AR’s coronal magnetic field with a widely used non-linear force-free method. This enables us to compute the RFLH using two independent gauge conditions for the vector potentials. We focus our study on the times of strong flares in the ARs, above the M class, and in regions around the polarity inversion lines (PILs) of the magnetic field, and of RFLH.
Results. We find that the temporal profiles of the relative helicity that is contained in the magnetic PIL follow those of the relative helicity that is computed by the accurate volume method for the whole AR. Additionally, the PIL relative helicity can be used to define a parameter similar to the well-known parameter R, whose high values are related with increased flaring probability. This helicity-based R-parameter correlates closely with the original parameter, showing in some cases even higher values. Additionally, it experiences more pronounced decreases during flares. This means that there exists at least one parameter deduced from RFLH that is important as a solar eruptivity indicator.
Key words: magnetohydrodynamics (MHD) / methods: numerical / Sun: flares / Sun: fundamental parameters / Sun: magnetic fields
© The Authors 2024
Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
This article is published in open access under the Subscribe to Open model. Subscribe to A&A to support open access publication.
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.