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Recurrent CME-like eruptions in emerging flux regions. II. Scaling of energy and collision of successive eruptions

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Syntelis_2019_ApJ_876_61.pdf (2.607Mb)
Date
03/05/2019
Author
Syntelis, P.
Archontis, V.
Tsinganos, K.
Funder
Science & Technology Facilities Council
Grant ID
ST/N000609/1
Keywords
Magnetohydrodynamics (MHD)
Methods: numerical
Sun: activity
Sun: interior
Sun: magnetic fields
QB Astronomy
NDAS
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Abstract
We present results of three-dimensional MHD simulations of recurrent eruptions in emerging flux regions. The initial numerical setup is the same as that in the work by Syntelis et al. Here, we perform a parametric study on the magnetic field strength (B 0) of the emerging field. The kinetic energy of the produced ejective eruptions in the emerging flux region ranges from 1026 to 1028 erg, reaching up to the energies of small coronal mass ejections. The kinetic and magnetic energies of the eruptions scale linearly in a logarithmic plot. We find that the eruptions are triggered earlier for higher B 0 and that B 0 is not directly correlated to the frequency of occurrence of the eruptions. Using large numerical domains, we show the initial stage of the partial merging of two colliding erupting fields. The partial merging occurs partly by the reconnection between the field lines of the following and the leading eruption at the interface between them. We also find that tether-cutting reconnection of the field lines of the leading eruption underneath the following eruption magnetically links the two eruptions. Shocks develop inside the leading eruption during the collision.
Citation
Syntelis , P , Archontis , V & Tsinganos , K 2019 , ' Recurrent CME-like eruptions in emerging flux regions. II. Scaling of energy and collision of successive eruptions ' , Astrophysical Journal , vol. 876 , no. 1 , 61 . https://doi.org/10.3847/1538-4357/ab16d2
Publication
Astrophysical Journal
Status
Peer reviewed
DOI
https://doi.org/10.3847/1538-4357/ab16d2
ISSN
1538-4357
Type
Journal article
Rights
Copyright © 2019. The American Astronomical Society. All rights reserved. This work is made available online in accordance with the publisher’s policies. This is the final published version of the work, which was originally published at: https://doi.org/10.3847/1538-4357/ab16d2
Description
This project has received funding from the Science and Technology Facilities Council (UK) through the consolidated grant ST/N000609/1. The authors acknowledge support by the Royal Society. This work was supported by computational time granted from the Greek Research & Technology Network (GRNET) in the National HPC facility—ARIS.
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  • University of St Andrews Research
URI
http://hdl.handle.net/10023/17758

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