The partial donor cell method

Hain, K.

doi:10.1016/0021-9991(87)90110-0

Cited by 95 publications

(68 citation statements)

References 8 publications

(1 reference statement)

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“…ISM is a large-scale magneto-hydrodynamic (MHD) code developed by Mission Research Corporation to simulate the magnetosphere-ionosphere system from its front boundary 40 R E upstream in the solar wind, to the base of the ionosphere near the Earth, and to deep in the magnetotail (White et al, 2001). Lacking the microphysics and resolution needed to accurately portray merging, ISM accomplishes the process through dissipation, either explicitly introduced by current dependent resistivity, or introduced by the code through the partial donor method (PDM) of Hain (1987), to maintain stability in the presence of steep gradients (see White et al, 2001, for more details). Through simulations of steady-state conditions or of responses to step-function driver variations, cause and effect relationships are easily isolated.…”

Section: Analysis Methodsmentioning

confidence: 99%

Polar, Cluster and SuperDARN evidence for high-latitude merging during southward IMF: temporal/spatial evolution

Maynard¹,

Ober²,

Burke

et al. 2003

Ann. Geophys.

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Abstract. Magnetic merging on the dayside magnetopause often occurs at high latitudes. Polar measured fluxes of accelerated ions and wave Poynting vectors while skimming the subsolar magnetopause. The measurements indicate that their source was located to the north of the spacecraft, well removed from expected component merging sites. This represents the first use of wave Poynting flux as a merging discriminator at the magnetopause. We argue that wave Poynting vectors, like accelerated particle fluxes and the Walén tests, are necessary, but not sufficient, conditions for identifying merging events. The Polar data are complemented with nearly simultaneous measurements from Cluster in the northern cusp, with correlated observations from the Super-DARN radar, to show that the locations and rates of merging vary. Magnetohydrodynamic (MHD) simulations are used to place the measurements into a global context. The MHD simulations confirm the existence of a high-latitude merging site and suggest that Polar and SuperDARN observed effects are attributable to both exhaust regions of a temporally varying X-line. A survey of 13 merging events places the location at high latitudes whenever the interplanetary magnetic field (IMF) clock angle is less than ∼150 • . While inferred highlatitude merging sites favor the antiparallel merging hypothesis, our data alone cannot exclude the possible existence of a guide field. Merging can even move away from equatorial latitudes when the IMF has a strong southward component. MHD simulations suggest that this happens when the dipole tilt angle increases or when IMF B X increases the effective dipole tilt.

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Section: Analysis Methodsmentioning

confidence: 99%

Polar, Cluster and SuperDARN evidence for high-latitude merging during southward IMF: temporal/spatial evolution

Maynard¹,

Ober²,

Burke

et al. 2003

Ann. Geophys.

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“…The ideal MHD equations [Chen, 1984], numerically solved by the partial donor method [Hain, 1977[Hain, , 1987, are used to model solar wind and magnetospheric plasmas. The ionosphere is simulated by solving a height integrated electrostatic equation that has been coupled via empirical relationships to the magnetospheric simulation.…”

Section: Code Descriptionmentioning

confidence: 99%

MHD simulation of the magnetotail during the December 10, 1996, substorm

Wiltberger¹,

Pulkkinen

Lyon³

et al. 2000

J. Geophys. Res.

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Abstract. This paper presents results of a global MHD simulation of a substorm that occurred on December 10, 1996. We concentrate on the relationship between the simulation results and the magnetotail observations during the growth and expansion phases of the substorm. In general, we find excellent agreement between the single point observations made by various spacecraft in both the geosynchronous and mid-tail regions: the simulation accurately represented the energy loading (lobe field increase), small-scale activations (partial dipolarizations), and a global substorm onset (large dipolarizations and fast flows). The global view presented by the simulation shows complex series of discrete flow channels during the expansion phase prior to the onset of global reconnection. It is these flows channels that disrupt the thin current sheets present during the expansion phase of the substorm.

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“…The coefficients of viscosity and resistivity are constant in space and time. Dissipation for numerical stability is encoded in the form of a partial donor cell method (PDM) [Hain, 1987]. The topology described here is insensitive to variations in these parameters.…”

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confidence: 99%

The Magnetospheric Sash and the Cross‐Tail S

White¹,

Siscoe²,

Erickson³

et al. 1998

Geophysical Research Letters

111

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Abstract. As revealed in MHD simulation, the magnetospheric sash is a band of weak magnetic field that, for the usual case in which the IMF is approximately perpendicular to thi geomagnetic dipole, runs tailward along the highlatitude magnetopause flanks from one dayside cusp to the other, closing via the cross-tail neutral sheet. On the magnetopause flanks, it contains the magnetic separator line, at which all three topological types of field lines meet. Seen in a cross-sectional plane through the near-Earth tail, the magnetospheric sash takes the form of the cross-tail S, a weak-field feature comprised of the tail neutral sheet with diagonally symmetric extensions along the magnetopause flanks connecting it to the separator line. The cross-tail S is evident in the MHD results and in cross-sectional maps based on IMP 8 data. The magnetopause expression of the sash is latent in prior works that described the geometry of antiparallel fields across the magnetopause and the consequent cancellation of the fields within the magnetopause layer. The sash picture bears a strong resemblance to antiparallel merging geometry. A new global magnetospheric structureGlobal MHD simulation reveals a hitherto unrecognized global magnetospheric structure. It is perhaps best described as a low field strength feature that runs, ribbon like, from one dayside cusp tailward along one flank of the magnetopause, then through the near-Earth tail as the neutral sheet to the other magnetopause flank, along which it runs back to the other dayside cusp. In keeping with the tradition of using sartorial designations for magnetospheric plasma structures--e.g., hood, mantle, sheet, and belt--we propose calling this newly recognized ribbon-like feature the magnetospheric sash. Our purpose here is to use a particular MHD simulation to document the sash's geometry, to ground its existence in global magnetic topology, and to identify its presence in data and its adumbration in prior work. The ISM MHD codeBefore describing the sash, we give some details of the MHD code and the boundary and initial conditions of the simulation to be presented here.

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The partial donor cell method

Cited by 95 publications

References 8 publications

Polar, Cluster and SuperDARN evidence for high-latitude merging during southward IMF: temporal/spatial evolution

Polar, Cluster and SuperDARN evidence for high-latitude merging during southward IMF: temporal/spatial evolution

MHD simulation of the magnetotail during the December 10, 1996, substorm

The Magnetospheric Sash and the Cross‐Tail S

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