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Lookup NU author(s): Professor Tamara Rogers
This is the authors' accepted manuscript of an article that has been published in its final definitive form by Institute of Physics Publishing Ltd., 2017.
For re-use rights please refer to the publisher's terms and conditions.
Hot Jupiters have proven themselves to be a rich class of exoplanets which test our theories of planetary evolution and atmospheric dynamics under extreme conditions. Here, we present three-dimensional magnetohydrodynamic simulations and analytic results which demonstrate that a dynamo can be maintained in the thin, stably-stratified atmosphere of a hot Jupiter, independent of the presumed deep-seated dynamo. This dynamo is maintained by conductivity variations arising from strong asymmetric heating from the planets' host star. The presence of a dynamo significantly increases the surface magnetic field strength and alters the overall planetary magnetic field geometry, possibly affecting star-planet magnetic interactions.
Author(s): Rogers T, McElwaine JN
Publication type: Article
Publication status: Published
Journal: The Astrophysical Journal Letters
Print publication date: 01/06/2017
Online publication date: 26/05/2017
Acceptance date: 12/05/2017
Date deposited: 16/06/2017
ISSN (print): 2041-8205
ISSN (electronic): 2041-8213
Publisher: Institute of Physics Publishing Ltd.
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