Piecewise Parabolic Method on a Local Stencil for Magnetized Supersonic Turbulence Simulation

TL;DR

The paper introduces PPML, a high-order, low-dissipation numerical scheme for simulating magnetized supersonic turbulence, maintaining divergence-free magnetic fields and demonstrating high accuracy and stability in complex astrophysical flows.

Contribution

PPML is a novel local stencil variant of PPM that evolves interface states with Riemann invariants, enabling stable, divergence-free, high-accuracy MHD turbulence simulations without additional dissipation.

Findings

Successfully simulates 3D supersonic MHD turbulence

Maintains divergence-free magnetic fields with constrained transport

Demonstrates high accuracy and low dissipation in turbulence modeling

Abstract

Stable, accurate, divergence-free simulation of magnetized supersonic turbulence is a severe test of numerical MHD schemes and has been surprisingly difficult to achieve due to the range of flow conditions present. Here we present a new, higher order-accurate, low dissipation numerical method which requires no additional dissipation or local "fixes" for stable execution. We describe PPML, a local stencil variant of the popular PPM algorithm for solving the equations of compressible ideal magnetohydrodynamics. The principal difference between PPML and PPM is that cell interface states are evolved rather that reconstructed at every timestep, resulting in a compact stencil. Interface states are evolved using Riemann invariants containing all transverse derivative information. The conservation laws are updated in an unsplit fashion, making the scheme fully multidimensional. Divergence-free evolution of the magnetic field is maintained using the higher order-accurate constrained transport technique of Gardiner and Stone. The accuracy and stability of the scheme is documented against a bank of standard test problems drawn from the literature. The method is applied to numerical simulation of supersonic MHD turbulence, which is important for many problems in astrophysics, including star formation in dark molecular clouds. PPML accurately reproduces in three-dimensions a transition to turbulence in highly compressible isothermal gas in a molecular cloud model. The low dissipation and wide spectral bandwidth of this method make it an ideal candidate for direct turbulence simulations.