Speed of PARODY-JA 4.2 on three supercomputers of GENCI (France): Jean-Zay (IDRIS), Adastra (CINES) and Irene (TGCC)

The PARODY-JA MHD simulation code

PARODY-JA is a branching of the PARODY numerical code originally developed by Emmanuel Dormy and myself to simulate Boussinesq convection and magnetic induction in a rotating spherical shell. Since 2006 I have been steadily developing PARODY-JA to make it one of the fastest codes available (see above) for this type of problem. The code can be obtained upon request.

Dynamical magnetic field line imaging (DMFI)

DMFI is a numerical visualization algorithm written by J. Aubert, designed to track magnetic field lines in MHD numerical simulations. DMFI is described in

Aubert, Aurnou, Wicht: The magnetic structure of convection-driven numerical dynamos, Geophys. J. Int. 172, 945-956, 2008, doi: 10.1111/j.1365-246X.2007.03693.x.

You can download the MATLAB source code of DMFI by following this link.

A geomagnetic reversal imaged with DMFI (from Aubert et al. 2008)

An operational prediction for the geomagnetic field evolution 2015-2115

The numerical data for the future internal geomagnetic field evolution described in the publication

Aubert, J.: Geomagnetic forecasts driven by thermal wind dynamics in Earth’s core, Geophys. J. Int. 203, 1738-1751, 2015, doi: 10.1093/gji/ggv394

are available for download. The file format is as follows: the first column is the epoch, and the rest of each line describes the Gauss coefficients ordered in IGRF-format (increasing spherical harmonic degree first, see this reference for a description of Gauss coefficients and the IGRF format). These coefficients can be used freely - please quote Aubert 2015 (above) when using this data.

Main field coefficients up to spherical harmonic degree and order 13

Secular variation coefficients up to spherical harmonic degree and order 13