Physical conditions for Jupiter-like dynamo models

TL;DR

This study uses 66 numerical simulations to identify the interior conditions that produce Jupiter-like magnetic fields, emphasizing the importance of the dynamo region depth and convective magnetic Reynolds number profile.

Contribution

It provides new insights into the interior parameters influencing Jupiter-like magnetic fields, especially the dynamo region extent and the role of convective flow profiles.

Findings

Jupiter-like magnetic fields can arise from various interior models.

The dynamo region likely extends to about 95% of Jupiter's radius.

Secondary dynamo effects from equatorial jets can produce low-latitude magnetic patches.

Abstract

The Juno mission will measure Jupiter's magnetic field with unprecedented precision and provide a wealth of additional data that will allow to constrain the planet's interior structure and dynamics. Here we analyse 66 numerical simulations in order to explore the sensitivity of the dynamo-generated magnetic field to the planets interior properties. The degree l=4 field model VIP4 and up-to-date interior models based on ab initio simulations serve as benchmarks. Our results suggest that VIP4-like magnetic fields can be found for a number of different models. 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. Low Rayleigh number leads to strong axial dipole contribution while the axial dipole dominance is lost 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 factor is the convective magnetic Reynolds number profile Rmc(r), 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. We extrapolated our results to Jupiter and the result suggests that the Jovian dynamo extends to 95% of the planetary radius. The zonal flows in our simulations are dominated by an equatorial jet largely confined to the molecular layer. Where the jet reaches down to higher electrical conductivities, it is gives rise to a secondary alpha-Omega dynamo that modifies the dipole-dominated field produced deeper in the planet. This secondary dynamo can lead to strong magnetic field patches at low latitudes that seem compatible with the VIP4 model.