Browse by author
Lookup NU author(s): Yasin Qazi, Professor Anvar ShukurovORCiD, Dr Devika Tharakkal, Dr Fred Gent
This work is licensed under a Creative Commons Attribution 4.0 International License (CC BY 4.0).
© 2023 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society. Stratified discs with strong horizontal magnetic fields, are susceptible to magnetic buoyancy instability (MBI). Modifying the magnetic field and gas distributions, this can play an important role in galactic evolution. The MBI and the Parker instability, in which MBI is exacerbated by cosmic rays, are often studied using an imposed magnetic field. However, in galaxies and accretion discs, the magnetic field is continuously replenished by a large-scale dynamo action. Using non-ideal MHD equations, we model a section of the galactic disc (we neglect rotation and cosmic rays considered elsewhere), in which the large-scale field is generated by an imposed α-effect of variable intensity to explore the interplay between dynamo instability and MBI. The system evolves through three distinct phases: the linear (kinematic) dynamo stage, the onset of linear MBI when the magnetic field becomes sufficiently strong and the non-linear, statistically steady state. Non-linear effects associated with the MBI introduce oscillations which do not occur when the field is produced by the dynamo alone. The MBI initially accelerates the magnetic field amplification but the growth is quenched by the vertical motions produced by MBI. We construct a 1D model, which replicates all significant features of 3D simulations to confirm that magnetic buoyancy alone can quench the dynamo and is responsible for the magnetic field oscillations. Unlike similar results obtained with an imposed magnetic field, the non-linear interactions do not reduce the gas scale height, so the consequences of the magnetic buoyancy depend on how the magnetic field is maintained.
Author(s): Qazi Y, Shukurov A, Tharakkal D, Gent FA, Bendre AB
Publication type: Article
Publication status: Published
Journal: Monthly Notices of the Royal Astronomical Society
Year: 2024
Volume: 527
Issue: 3
Pages: 7994-8005
Print publication date: 01/01/2024
Online publication date: 01/12/2023
Acceptance date: 27/11/2023
Date deposited: 04/01/2024
ISSN (print): 0035-8711
ISSN (electronic): 1365-2966
Publisher: Oxford University Press
URL: https://doi.org/10.1093/mnras/stad3684
DOI: 10.1093/mnras/stad3684
Data Access Statement: The raw data for this work were obtained from numerical simulations using the open source pencil code available at https://github.com/pencil-code/pencil-code.git. The derived data used for the analysis given in the paper is available on request from the corresponding author.
Altmetrics provided by Altmetric
