3 edition of **A numerical code for a three-dimensional magnetospheric MHD equilibrium model** found in the catalog.

A numerical code for a three-dimensional magnetospheric MHD equilibrium model

G. H. Voigt

- 231 Want to read
- 31 Currently reading

Published
**1992**
by National Aeronautics and Space Administration, National Technical Information Service, distributor in [Washington, DC], Springfield, Va.?
.

Written in English

- Magnetosphere -- Mathematical models.

**Edition Notes**

Other titles | A Nnumerical code for a three dimensional magnetospheric MHD equilibrium model. |

Statement | principal investigator: G.-H. Voigt. |

Series | NASA-CR -- 189852., NASA contractor report -- NASA CR-189852. |

Contributions | United States. National Aeronautics and Space Administration. |

The Physical Object | |
---|---|

Format | Microform |

Pagination | 1 v. |

ID Numbers | |

Open Library | OL17676597M |

Modeling the Inner Magnetosphere with the Coupled Rice Convection Model – Equilibrium Code C. Lemon 1*, T. W and A Schlüter, A 3D code for MHD equilibrium and stability, J. Comput Rich, and M. Smiddy, Quantitative simulation of a magnetospheric substorm 1, model logic and overview, J. Geophys. Res., 86, , a. Hesse, M Cited by: 1. three-dimensional MHD fluid-gyrokinetic particle hybrid code, a three-dimensional MHD version of the code in generalized orthogonal coordinates has been developed The new code was used with a model for the Neglecting all kinetic effects and using a self-consistent MHD equilibrium obtained from a multiscale perturbation expansion of.

@article{osti_, title = {Three-dimensional nonlinear ideal MHD equilibria with field-aligned incompressible and compressible flows}, author = {Moawad, S. M., E-mail: [email protected] and Ibrahim, D. A.}, abstractNote = {The equilibrium properties of three-dimensional ideal magnetohydrodynamics (MHD) are investigated.. Incompressible and compressible flows are. Self‐consistent inner magnetosphere simulation driven by a global MHD model global three‐dimensional magnetospheric MHD code in order to try to reproduce the full kinetic physics. There have been magnetic flux boundaries for the equilibrium code using empirical magnetic field models such as T89 [Tsyganenko,Cited by:

The Riemann problem for two-dimensional gas dynamics with isentropic or polytropic gas is considered. The initial data is constant in each quadrant and chosen so that only a rarefaction wave, shock wave, or slip line connects two neighboring constant initial by: Coupling of a global MHD code and an inner magnetospheric model: Initial results Darren L. De Zeeuw Center for Space Environment Modeling, University of Michigan, Ann Arbor, Michigan, USA Stanislav Sazykin and Richard A. Wolf Department of Physics and Astronomy, Rice University, Houston, Texas, USA Tamas I. Gombosi, Aaron J. Ridley, and Gabor Cited by:

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Abstract Two dimensional and three dimensional MHD equilibrium models were begun for Earth's magnetosphere. The original proposal was motivated by realizing that global, purely data based models of Earth's magnetosphere are inadequate for studying the underlying plasma physical principles according to which the magnetosphere evolves on the quasi-static convection time scale.

Get this from a library. A numerical code for a three-dimensional magnetospheric MHD equilibrium model. [G H Voigt; United States. National Aeronautics and Space Administration.]. Two dimensional and three dimensional MHD equilibrium models were begun for Earth's magnetosphere.

The original proposal was motivated by realizing that global, purely data based models of Earth's magnetosphere are inadequate for studying the underlying plasma physical principles according to which the magnetosphere evolves on the quasi-static convection time scale.

Complex numerical. "A Numerical Code for a Three-Dimensional Magnetospheric MHD Equilibrium Model" (prepared on Febru by G.-H. Voigt) Report Summary Title: A Numerical Code for a Three-Dimensional Magnetospheric MHD Equilibrium Model Principal Investigator: G.-H.

Voigt; Institution: Rice University. This is a summary report of a two-year grant. A three-dimensional magnetospheric equilibrium code, the MAG-3D code, has been developed by employing an iterative metric method. The main difference between the three-dimensional and the two-dimensional axisymmetric solutions is that the field-aligned current and the toroidal magnetic field are finite for the three-dimensional case, but vanish Author: C.Z.

Cheng. We have simulated the steady state magnetospheric configuration which results when solar wind plasma impinges on a magnetic dipole. In our calculation, the MHD equations were solved self-consistently by a large scale code which employs Rusanov's method to produce a three-dimensional model.

We present results from a modified MHD code that is used to compute global three-dimensional force equilibria in the Earth's magnetosphere. A nonuniform rectilinear grid is used along with initial conditions supplied by empirical magnetic field and pressure models. These initial conditions do not, in general, satisfy the force balance condition J × B = p.

The MagnetoFriction code solves the. [1] A new Euler potential method is presented for computing 3‐D magnetospheric equilibria with prescribed plasma pressure, that significantly improves on a previous flux coordinate approach. In the new approach, the Euler potential α is no longer necessarily the magnetic flux, but can be specified much more freely, allowing equilibrium calculations in much more extended magnetospheric by: The ideal MHD model also constitutes the model for developing the theory of wave propagation in a plasma.

While the conservative formulation given by equations (), (), (), and () can be attractive from the numerical point of view, a more convenient form of the governing equation can be obtained by reformulating the. Proceedings of ISSS-7, March, Magnetospheric equilibrium including the near-Earth region and the magnetotail Sorin Zaharia 1, J.

Birn, and C. Cheng2 1Space Science and Applications, Los Alamos National Laboratory, Los Alamos, NM, USA 2Princeton Plasma Physics Laboratory, Princeton University, Princeton, NJ, USA We present a ﬁrst step in developing a realistic global. MHD simulations started at the end of the s, and the initial study was limited to two-dimensional (2D) cases.

Due to the intrinsic three-dimensional (3D) characteristics of the geospace, 3D MHD simulations emerged in the s, in an attempt to model the large-scale structures and fundamental physical processes in the magnetosphere.

Toward a global magnetospheric equilibrium model Sorin Zaharia and J. Birn In general (5) and (6) are three-dimensional equations.

However, in the {a, b, c} system we can reduce boundary conditions for a and b as well as the P(a, b) distribution at an arbitrary location on each field line. [14] A numerical 3-D code has been developed to Cited by: 6. Chebyshev-ваsed solvers for three-dimensional elliptic equations.

(INVITED TALK) – V.A. Protasov, I.S. Ulyanichev, I.M. Gubaydullin A new high-order accuracy numerical method for numerical modeling of supernovae explosions.

– I.M. Kulikov The numerical modeling of the collapse of molecular cloud on adaptive nested. A three-dimensional magnetospheric equilibrium code, the MAG-3D code, has been developed by employing an iterative metric method.

The MAG-3D code is Author: Sorin Zaharia. A three-dimensional magnetospheric equilibrium code, the MAG-3D code, has been developed by employing an iterative metric method. The MAG-3D code is. This is not a severe limitation for the considered applications, because numerical accu- racy anyway requires a time step of that order.

For several purposes a Lax step is incorporated in 80 A. Otto / 3D resistive MHD computations of magnetospheric physics the MHD by: guiding-centers.

A new numerical simulation code for solving a reduced Vlasov equation in ﬁve-dimensions as well as Maxwell equations is developed.

We demonstrate that the present model is capable of describing the propagation of magnetohydrodynamic (MHD) waves as. We review a long-standing effort at Rice University in magnetospheric modeling with the Rice Convection Model.

After briefly describing the basic assumptions and equations that make up the core of the RCM, we present a sampling of recent results using the model. We conclude with a brief description of ongoing and future improvements to the RCM.

et al. The basic equations and numerical methods are essentially the same as those in Iijima & Yokoyama (). Additional details of the numerical methods are described in Iijima (). We conduct a simulation with a three-dimensional numerical domain spanning 9 9 16 Mm3, including the upper convection zone with a depth of 2 Mm.

the -model (Shakura & Sunyaev ; Novikov & Thorne ), and controls the accretion rate through the disk. To model accretion, the ideal MHD equations are solved numer-ically in three dimensions, using a Godunov-type numerical code, written in a “cubed-sphere” coordinate system rotating with the star (Koldoba et al.

; Romanova et al. motions. The driving generates various MHD modes within the ﬂux tube and acoustic waves in the ambient medium. We study the propagation and other properties of MHD modes generated by these drivers. Section 2 discusses the construction of the initial magneto-hydrostatic equilibrium model and the proper-ties of the model.

The excitation.We present the results of a three dimensional global magnetohydrodynamic (MHD) model of the magnetosphere of Saturn. The model represents the interaction of a magnetized solar wind with a fast rotating, magnetized planet and includes planetary rotation as well as a simplified model of the neutral torus produced by by: Numerical Methods for 3-dimensional Magnetic Conﬁnement Conﬁgurations using Two-Fluid Plasma Equations Bhuvana Srinivasan Chair of the Supervisory Committee: Professor Uri Shumlak Aeronautics & Astronautics The 5-moment two-ﬂuid plasma model uses .