User Manual Privacy Policy Disclaimer Contact us
  Advanced SearchBrowse


  Physical conditions for Jupiter-like dynamo models

Duarte, L. D., Wicht, J., & Gastine, T. (2018). Physical conditions for Jupiter-like dynamo models. Icarus, 299, 206-221. doi:10.1016/j.icarus.2017.07.016.

Item is


show hide
Item Permalink: http://hdl.handle.net/21.11116/0000-0003-31F3-3 Version Permalink: http://hdl.handle.net/21.11116/0000-0003-31F4-2
Genre: Journal Article


show Files




Duarte, Lúcia D.V., Author
Wicht, Johannes1, Author              
Gastine, Thomas, Author
1Department Planets and Comets, Max Planck Institute for Solar System Research, Max Planck Society, ou_1832288              


Free keywords: Atmospheres Dynamics Jupiter Interior Variable electrical conductivity Numerical dynamos
 Abstract: The Juno mission will measure Jupiter’s magnetic field with unprecedented precision and provide a wealth of additional data that will allow us to constrain the planet’s interior structure and dynamics. Here we analyse 66 different numerical simulations in order to explore the sensitivity of the dynamo-generated magnetic field to the planets interior properties. Jupiter field models based on pre-Juno data and up-to-date interior models based on ab initio simulations serve as benchmarks. Our results suggest that Jupiter-like magnetic fields can be found for a number of different models. These complement the steep density gradients in the outer part of the simulated shell with an electrical conductivity profile that mimics the low conductivity in the molecular hydrogen layer and thus renders the dynamo action in this region largely unimportant. We find that whether we assume an ideal gas or use the more realistic interior model based on ab initio simulations makes no difference. However, two other factors are important. A low Rayleigh number leads to a too strong axial dipole contribution while the axial dipole dominance is lost altogether when the convective driving is too strong. The required intermediate range that yields Jupiter-like magnetic fields depends on the other system properties. The second important factor is the convective magnetic Reynolds number radial profile Rmc(r), basically a product of the non-axisymmetric flow velocity and electrical conductivity. We find that the depth where Rmc exceeds about 50 is a good proxy for the top of the dynamo region. When the dynamo region sits too deep, the axial dipole is once more too dominant due to geometric reasons. Extrapolating our results to Jupiter and the result suggests that the Jovian dynamo extends to 95% of the planetary radius. The zonal flow system in our simulations is dominated by an equatorial jet which remains largely confined to the molecular layer. Where the jet reaches down to higher electrical conductivities, however, it gives rise to a secondary αΩ dynamo that modifies the dipole-dominated field produced deeper in the planet. This secondary dynamo can lead to strong magnetic field patches at lower latitudes that seem compatible with the pre-Juno field models.


Language(s): eng - English
 Dates: 2019-03-192018
 Publication Status: Published in print
 Pages: -
 Publishing info: -
 Table of Contents: -
 Rev. Type: Peer
 Identifiers: DOI: 10.1016/j.icarus.2017.07.016
 Degree: -



Legal Case


Project information


Source 1

Title: Icarus
Source Genre: Journal
Publ. Info: Amsterdam : Academic Press
Pages: - Volume / Issue: 299 Sequence Number: - Start / End Page: 206 - 221 Identifier: ISSN: 0019-1035
CoNE: https://pure.mpg.de/cone/journals/resource/954922645023