Browse by author
Lookup NU author(s): Dr Luke Chamandy,
Professor Anvar ShukurovORCiD
Full text for this publication is not currently held within this repository. Alternative links are provided below where available.
Galactic magnetic arms have been observed between the gaseous arms of some spiral galaxies; their origin remains unclear. We suggest that magnetic spiral arms can be naturally generated in the interarm regions because the galactic fountain flow or wind is likely to be weaker there than in the arms. Galactic outflows lead to two countervailing effects: removal of small-scale magnetic helicity, which helps to avert catastrophic quenching of the dynamo, and advection of the large-scale magnetic field, which suppresses dynamo action. For realistic galactic parameters, the net consequence of outflows being stronger in the gaseous arms is higher saturation large-scale field strengths in the interarm regions as compared to in the arms. By incorporating rather realistic models of spiral structure and evolution into our dynamo models, an interlaced pattern of magnetic and gaseous arms can be produced.
Author(s): Chamandy L, Shukurov A, Subramanian K
Publication type: Article
Publication status: Published
Journal: Monthly Notices Letters of the Royal Astronomical Society
Print publication date: 01/01/2015
Online publication date: 17/10/2014
Acceptance date: 16/09/2014
ISSN (print): 0035-8711
ISSN (electronic): 1365-2966
Publisher: Oxford University Press
Altmetrics provided by Altmetric