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Title:
Smoothed Particle Magnetohydrodynamics - III. Multidimensional tests and the ∇.B= 0 constraint
Authors:
Price, D. J.; Monaghan, J. J.
Affiliation:
AA(School of Physics, University of Exeter, Stocker Road, Exeter EX4 4QL), AB(School of Mathematical Sciences, Monash University, Clayton 3800, Australia)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 364, Issue 2, pp. 384-406. (MNRAS Homepage)
Publication Date:
12/2005
Origin:
MNRAS
MNRAS Keywords:
magnetic fields, MHD, methods: numerical, stars: formation
DOI:
10.1111/j.1365-2966.2005.09576.x
Bibliographic Code:
2005MNRAS.364..384P

Abstract

In two previous papers (Papers I and II), we have described an algorithm for solving the equations of Magnetohydrodynamics (MHD) using the Smoothed Particle Hydrodynamics (SPH) method. The algorithm uses dissipative terms in order to capture shocks and has been tested on a wide range of one-dimensional problems in both adiabatic and isothermal MHD. In this paper, we investigate multidimensional aspects of the algorithm, refining many of the aspects considered in Papers I and II and paying particular attention to the code's ability to maintain the ∇.B= 0 constraint associated with the magnetic field. In particular, we implement a hyperbolic divergence cleaning method recently proposed by Dedner et al. in combination with the consistent formulation of the MHD equations in the presence of non-zero magnetic divergence derived in Papers I and II. Various projection methods for maintaining the divergence-free condition are also examined. Finally, the algorithm is tested against a wide range of multidimensional problems used to test recent grid-based MHD codes. A particular finding of these tests is that in Smoothed Particle Magnetohydrodynamics (SPMHD), the magnitude of the divergence error is dependent on the number of neighbours used to calculate a particle's properties and only weakly dependent on the total number of particles. Whilst many improvements could still be made to the algorithm, our results suggest that the method is ripe for application to problems of current theoretical interest, such as that of star formation.

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