## A fully self-consistent multi-layered model of Jupiter

##### View/Open

2016_ApJ_Vol 826_pp 127.pdf (1.801Mb)
##### Date

2016-07-27##### Author

Kong, D

Zhang, K

Schubert, G

##### Date issued

2016-07-27

##### Journal

Astrophysical Journal

##### Type

Article

##### Language

en

##### Publisher

American Astronomical Society

##### Rights

This is the final version of the article. Available from American Astronomical Society via the DOI in this record.

##### Abstract

We construct a three-dimensional, fully self-consistent, multi-layered, non-spheroidal model of Jupiter consisting of an inner core, a metallic electrically conducting dynamo region, and an outer molecular electrically insulating envelope. We assume that the Jovian zonal winds are on cylinders parallel to the rotation axis but, due to the effect of magnetic braking, are confined within the outer molecular envelope. We also assume that the location of the molecular-metallic interface is characterized by its equatorial radius ${{HR}}_{e}$, where R e is the equatorial radius of Jupiter at the 1 bar pressure level and H is treated as a parameter of the model. We solve the relevant mathematical problem via a perturbation approach. The leading-order problem determines the density, size, and shape of the inner core, the irregular shape of the 1 bar pressure level, and the internal structure of Jupiter that accounts for the full effect of rotational distortion, but without the influence of the zonal winds; the next-order problem determines the variation of the gravitational field solely caused by the effect of the zonal winds on the rotationally distorted non-spheroidal Jupiter. The leading-order solution produces the known mass, the known equatorial and polar radii, and the known zonal gravitational coefficient J 2 of Jupiter within their error bars; it also yields the coefficients J 4 and J 6 within about 5% accuracy, the core equatorial radius $0.09{R}_{e}$ and the core density ${\rho }_{c}=2.0\times {10}^{4}\,{\rm{kg}}\,{{\rm{m}}}^{-3}$ corresponding to 3.73 Earth masses; the next-order solution yields the wind-induced variation of the zonal gravitational coefficients of Jupiter.

##### Funders/Sponsor

K.Z. is supported by Leverhulme Trust Research Project Grant RPG-2015-096 and by Macau FDCT grants 039/2013/A2 and 007/2016/A1. The computation made use of the high performance computing resources in the Core Facility for Advanced Research Computing at Shanghai Astronomical Observatory, Chinese Academy of Sciences.

##### Citation

Vol. 826, No. 2, pp. 127 - 134

##### EISSN

1538-4357

##### ISSN

0004-637X