Volume 545, September 2012
|Number of page(s)||16|
|Section||Numerical methods and codes|
|Published online||25 September 2012|
A conservative orbital advection scheme for simulations of magnetized shear flows with the PLUTO⋆ code
1 Dipartimento di Fisica GeneraleUniversitá di Torino, via Pietro Giuria 1, 10125 Torino, Italy
2 CEA Irfu, SAP, Centre de Saclay, 91191 Gif-sur-Yvette, France
3 Max Planck Institute for Astronomy, Königstuhl 17, 69117 Heidelberg, Germany
4 Institute for Astronomy and Astrophysics, Section Computational Physics, Eberhard Karls Universität Tübingen, Auf der Morgenstelle 10, 72076 Tübingen, Germany
e-mail: firstname.lastname@example.org; email@example.com
5 Consorzio Interuniversitario CINECA, via Magnanelli 6/3, 40033 Casalecchio di Reno, Bologna, Italy
Received: 8 May 2012
Accepted: 29 June 2016
Context. Explicit numerical computations of hypersonic or super-fast differentially rotating disks are subject to the time-step constraint imposed by the Courant condition, according to which waves cannot travel more than a fraction of a cell during a single time-step update. When the bulk orbital velocity largely exceeds any other wave speed (e.g., sound or Alfvén), as computed in the rest frame, the time step is considerably reduced and an unusually large number of steps may be necessary to complete the computation.
Aims. We present a robust numerical scheme to overcome the Courant limitation by improving and extending the algorithm previously known as FARGO (fast advection in rotating gaseous objects) to the equations of magnetohydrodynamics (MHD) using a more general formalism. The proposed scheme conserves total angular momentum and energy to machine precision and works in cartesian, cylindrical, or spherical coordinates. The algorithm has been implemented in the next release of the PLUTO code for astrophysical gasdynamics and is suitable for local or global simulations of accretion or proto-planetary disk models.
Methods. By decomposing the total velocity into an average azimuthal contribution and a residual term, the algorithm approaches the solution of the MHD equations through two separate steps corresponding to a linear transport operator in the direction of orbital motion and a standard nonlinear solver applied to the MHD equations written in terms of the residual velocity. Since the former step is not subject to any stability restriction, the Courant condition is computed only in terms of the residual velocity, leading to substantially larger time steps. The magnetic field is advanced in time using the constrained transport method in order to fulfill the divergence-free condition. Furthermore, conservation of total energy and angular momentum is enforced at the discrete level by properly expressing the source terms in terms of upwind Godunov fluxes available during the standard solver.
Results. Our results show that applications of the proposed orbital-advection scheme to problems of astrophysical relevance provides, at reduced numerical cost, equally accurate and less dissipative results than standard time-marching schemes.
Key words: methods: numerical / accretion, accretion disks / protoplanetary disks / magnetohydrodynamics (MHD) / turbulence
Freely distributed at http://plutocode.ph.unito.it.
© ESO, 2012
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