Finite Volume TVD Scheme on an Unstructured Grid System for Three-Dimensional MHD Simulation of Inhomogeneous Systems Including Strong Background Potential Fields

Tanaka, Takashi

doi:10.1006/jcph.1994.1071

Cited by 274 publications

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“…Owing to this problem the adoption of unstructured grid is unavoidable. The MHD scheme used in this paper employs the finite volume (FV) total-variation diminishing (TVD) scheme to cope with the unstructured grid system and to achieve a highly accurate analysis including an excellent discontinuity capturing [Tanaka, 1994].…”

Section: Simulation Methodsmentioning

confidence: 99%

“…Therefore the ratio of variable to intrinsic components of the magnetic field becomes extremely small in the ionosphere. In order to avoid this difficulty, the MHD equations are reconstructed by dividing B as B = B 0 + B 1 , where B 0 and B 1 are known intrinsic and unknown variable components, respectively [Tanaka, 1994]. In the S-M-I interaction problem treated in this paper, B 0 adopts a dipole field whose axis is in the z direction.…”

Section: Simulation Methodsmentioning

confidence: 99%

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Formation of magnetospheric plasma population regimes coupled with the dynamo process in the convection system

Tanaka

2003

J. Geophys. Res.

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[1] Based on the magnetosphere-ionosphere (M-I) coupling scheme, convection as a compound system is considered including the generation of plasma population regimes in the magnetosphere. In these considerations, primary elements that must be set to a selfconsistent configuration are convection flows in the magnetosphere and the ionosphere, field-aligned current (FAC) systems, ionospheric currents, energy conversion processes, and plasma population regimes. The convection in the M-I coupling system is inextricably associated with the FACs. In the present results, the region-1 and region-2 FACs are driven by rP current inside the magnetosphere through plasma internal energy accumulated in the cusp and plasma sheet, respectively. In this process, mechanisms to drive the region-1 and region-2 FACs are the same two-step process; tangential Maxwell stress on the magnetopause pumps up plasma internal energy inside the magnetosphere, then plasma internal energy drives the FACs. This dynamo can be driven by a steady convection flow which is suitable to project down to the low-b regions. Thus from the magnetohydrodynamic (MHD) force balance controlling the convection, plasma population regimes appear through a requirement to form dynamo in the magnetosphere, showing that plasma population regimes are indispensable to fulfill the self-consistency in the convection system. In the model that the convection is driven directly by the linetying current, the shoulder of the magnetosphere behind the cusp, where the line-tying current is mixed with the pure Chapman-Ferraro current connected to dayside, constructs the dynamo (J.E < 0) for the region-1 FAC. In the present model with negative IMF B z , on the contrary, the Chapman-Ferraro current in this area is not directly connected with the region-1 FAC but connected with the neutral sheet current in the dayside merging region to increase plasma internal energy (J.E > 0) around the cusp. Similarly, tail theta current system acts to increase plasma internal energy in the plasma sheet through the convection. The magnetospheric model derived from this consideration enables a continuous switch over from the confinement state of geomagnetic field in the ChapmanFerraro model to the convection of Dungey model for nonzero IMF B z . In the present convection model, nearly force-free open field lines are extending from the polar cap into the lobes. Based on the convection model proposed in this paper, a suggestion is given for the substorm models in the next decade that they must develop from a modular model to a globally self-consistent model. Citation: Tanaka, T., Formation of magnetospheric plasma population regimes coupled with the dynamo process in the convection system,

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Section: Simulation Methodsmentioning

confidence: 99%

Section: Simulation Methodsmentioning

confidence: 99%

Formation of magnetospheric plasma population regimes coupled with the dynamo process in the convection system

Tanaka

2003

J. Geophys. Res.

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“…The calculation for MHD equations employs the finite volume method (FVM) with an upwinding numerical flux. To obtain a higher order of accuracy, the third-order total variation diminishing (TVD) numerical flux is used on the basis of the monotonic upstream scheme for conservation laws (MUSCL) approach [Tanaka, 1994]. The grid structure is designed so as to obtain sufficient resolutions both in the inner magnetosphere and in the tail region.…”

Section: Modelmentioning

confidence: 99%

Configuration of the magnetosphere‐ionosphere convection system under northward IMF conditions with nonzero IMF B_y

Tanaka¹

1999

J. Geophys. Res.

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“…In the fully conservative scheme the problem occurring in regions where the magnetic field is very strong can be avoided by solving only for the deviation of the magnetic field from the intrinsic magnetic field. This method was introduced by Tanaka (1994), and has also been used in the BATS-R-US code and in the Lyon/Fedder code. In addition to the above equations the condition ∇ ⋅ B = 0 has to be satisfied throughout the numerical system.…”

Section: Magnetohydrodynamic Equationsmentioning

confidence: 99%

“…The Riemann solver is a Roe scheme (Roe, 1981). The Tanaka code is based on a Total-Variance-Diminishing scheme which works due to formulation by the finite volume method on an unstructured grid (Tanaka, 1994). A combination of the leapfrog scheme with the two-step Lax-Wendroff scheme is used by T. Ogino (e.g., Ogino et al, 1994) in his global code based on the non-conservative MHD equations.…”

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confidence: 99%

Space Storms and Space Weather Hazards

Daglis¹

2001

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Finite Volume TVD Scheme on an Unstructured Grid System for Three-Dimensional MHD Simulation of Inhomogeneous Systems Including Strong Background Potential Fields

Cited by 274 publications

References 0 publications

Formation of magnetospheric plasma population regimes coupled with the dynamo process in the convection system

Formation of magnetospheric plasma population regimes coupled with the dynamo process in the convection system

Configuration of the magnetosphere‐ionosphere convection system under northward IMF conditions with nonzero IMF B_y

Space Storms and Space Weather Hazards

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Finite Volume TVD Scheme on an Unstructured Grid System for Three-Dimensional MHD Simulation of Inhomogeneous Systems Including Strong Background Potential Fields

Cited by 274 publications

References 0 publications

Formation of magnetospheric plasma population regimes coupled with the dynamo process in the convection system

Formation of magnetospheric plasma population regimes coupled with the dynamo process in the convection system

Configuration of the magnetosphere‐ionosphere convection system under northward IMF conditions with nonzero IMF By

Space Storms and Space Weather Hazards

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Configuration of the magnetosphere‐ionosphere convection system under northward IMF conditions with nonzero IMF B_y