TY - JOUR
T1 - Modeling the Effects of a Light Bridge on Properties of Magnetohydrodynamic Waves in Solar Pores
AU - Schiavo, Luiz A. C. A.
AU - Gordovskyy, Mykola
AU - Browning, Philippa K.
AU - de Souza e Almeida Silva, Suzana
AU - Verth, Gary
AU - Ballai, Istvan
AU - Shelyag, Sergiy
AU - Ruzheinikov, Sergey N.
AU - McLaughlin, James A.
AU - Fedun, Viktor
N1 - © 2024. The Author(s). Published by the American Astronomical Society. This is an open access article distributed under the Creative Commons Attribution License, to view a copy of the license, see: https://creativecommons.org/licenses/by/4.0/
PY - 2024/11/1
Y1 - 2024/11/1
N2 - Solar pores are ideal magnetic structures for wave propagation and transport of energy radially outwards across the upper layers of the solar atmosphere. We aim to model the excitation and propagation of magnetohydrodynamic waves in a pore with a light bridge modeled as two interacting magnetic flux tubes separated by a thin, weaker-field layer. We solve the three-dimensional magnetohydrodynamic equations numerically and calculate the circulation as a measure of net torsional motion. We find that the interaction between flux tubes results in the natural excitation of propagating torsional Alfvén waves but find no torsional waves in the model with a single flux tube. The torsional Alfvén waves propagate with wave speeds matching the local Alfvén speed where wave amplitude peaks.
AB - Solar pores are ideal magnetic structures for wave propagation and transport of energy radially outwards across the upper layers of the solar atmosphere. We aim to model the excitation and propagation of magnetohydrodynamic waves in a pore with a light bridge modeled as two interacting magnetic flux tubes separated by a thin, weaker-field layer. We solve the three-dimensional magnetohydrodynamic equations numerically and calculate the circulation as a measure of net torsional motion. We find that the interaction between flux tubes results in the natural excitation of propagating torsional Alfvén waves but find no torsional waves in the model with a single flux tube. The torsional Alfvén waves propagate with wave speeds matching the local Alfvén speed where wave amplitude peaks.
KW - Solar physics
KW - Solar photosphere
KW - Magnetohydrodynamics
KW - Solar magnetic fields
KW - Solar oscillations
U2 - 10.3847/1538-4357/ad7958
DO - 10.3847/1538-4357/ad7958
M3 - Article
SN - 0004-637X
VL - 975
SP - 1
EP - 9
JO - The Astrophysical Journal
JF - The Astrophysical Journal
IS - 1
M1 - 45
ER -