Magnetic flux cancellation in a 3D magnetohydrodynamic simulation of an emerging flux tube with a non-uniform twist
Abstract
Flux emergence is often accompanied by flux cancellation, which may drive dynamic phenomena in the solar atmosphere. We studied magnetic flux cancellation in a three-dimensional resistive magnetohydrodynamic (MHD) simulation of an emerging flux tube with a non-uniform twist profile. We solved time-dependent resistive MHD equations to model flux emergence into a magnetised background atmosphere. We identified several cancellation sites, estimated their cancellation rates, and examined the magnetic topology and associated jet activity. The non-uniform twist produced multiple opposite photospheric polarities, leading to a complex multipolar magnetic configuration rather than a simple dipolar structure. Interactions between inner secondary magnetic patches resulted in flux cancellation of the photospheric Bz along their polarity inversion line (PIL). These interactions led to the formation of concave-up loops and a cancellation rate of 1.1 × 1019 Mx hr−1. During cancellation, magnetic reconnection between converging opposite polarities progressively created a coherent magnetic flux rope above the cancellation region. The evolution of the rope was associated with a blowout jet, as the rope expanded and released part of its stored twist into the overlying corona. We also examined two smaller secondary cancellation events at photospheric heights. Our results highlight the role of internal flux cancellation in restructuring the magnetic field and driving blowout-jet activity in emerging regions.
Versions
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BibTeX
@misc{agalianou2026magnetic,
title = {{Magnetic flux cancellation in a 3D magnetohydrodynamic simulation of an emerging flux tube with a non-uniform twist}},
author = {V. Agalianou and S. Patsourakos and V. Archontis},
howpublished = {arXiv},
year = {2026},
month = oct,
doi = {10.48550/arxiv.2610.11983},
eprint = {2610.11983},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2610.11983},
note = {CC BY 4.0},
}
RIS
TY - UNPB
TI - Magnetic flux cancellation in a 3D magnetohydrodynamic simulation of an emerging flux tube with a non-uniform twist
AU - V. Agalianou
AU - S. Patsourakos
AU - V. Archontis
PY - 2026
DA - 2026/10/08
PB - arXiv
DO - 10.48550/arxiv.2610.11983
UR - https://arxiv.org/abs/2610.11983
AB - Flux emergence is often accompanied by flux cancellation, which may drive dynamic phenomena in the solar atmosphere. We studied magnetic flux cancellation in a three-dimensional resistive magnetohydrodynamic (MHD) simulation of an emerging flux tube with a non-uniform twist profile. We solved time-dependent resistive MHD equations to model flux emergence into a magnetised background atmosphere. We identified several cancellation sites, estimated their cancellation rates, and examined the magnetic topology and associated jet activity. The non-uniform twist produced multiple opposite photospheric polarities, leading to a complex multipolar magnetic configuration rather than a simple dipolar structure. Interactions between inner secondary magnetic patches resulted in flux cancellation of the photospheric B_z along their polarity inversion line (PIL). These interactions led to the formation of concave-up loops and a cancellation rate of 1.1 × 10^19 Mx hr^−1. During cancellation, magnetic reconnection between converging opposite polarities progressively created a coherent magnetic flux rope above the cancellation region. The evolution of the rope was associated with a blowout jet, as the rope expanded and released part of its stored twist into the overlying corona. We also examined two smaller secondary cancellation events at photospheric heights. Our results highlight the role of internal flux cancellation in restructuring the magnetic field and driving blowout-jet activity in emerging regions.
ER -