A Free, Fast, Simple and Efficient TVD MHD Code

Details A Free, Fast, Simple and Efficient TVD MHD Code A Free, Fast, Simple and Efficient TVD MHD Code

2003-05-06

arxiv.org/abs/astro-ph/0305088v1

Astronomy and Astrophysics

Astrophysics

17 pages, 6 figures, submitted to the astrophysical journal

Scientific paper

We describe a numerical method to solve the magnetohydrodynamic (MHD) equations. The fluid variables are updated along each direction using the flux conservative, 2nd order, total variation diminishing (TVD), upwind scheme of Jin and Xin. The magnetic field is updated separately in two-dimensional advection-constraint steps. The electromotive force (EMF) is computed in the advection step using the TVD scheme, and this same EMF is used immediately in the constraint step in order to preserve \grad.B=0 without the need to store intermediate fluxes. Operator splitting is used to extend the code to three dimensions, and Runge-Kutta is used to get second order accuracy in time. The advantages of this code are high resolution per grid cell, second order accuracy in space and time, enforcement of the \grad.B=0 constraint to machine precision, no memory overhead, speed, and simplicity. A 3-D Fortran implementation less than 400 lines long is made freely available. We also implemented a fully scalable message-passing parallel MPI version. We present tests of the code on MHD waves and shocks.

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