Global numerical simulation of the growth phase and the expansion onset for a substorm observed by Viking

Fedder, J. A.; Slinker, S. P.; Lyon, J. G.; Elphinstone, R. D.

doi:10.1029/95ja01524

Cited by 154 publications

(162 citation statements)

References 17 publications

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“…A recent focus of MHD investigations is the study of of the magnetic cloud that forms, and CME plasma propermagnetospheric "events." In these simulations the observed upstream solar wind conditions to are used to "drive" the magnetosphere-ionosphere system, and numerical predictions are compared with ground based or satellite observations [Fedder et al, 1995b[Fedder et al, , 1998Raeder et al, 1998]. In adties.…”

mentioning

confidence: 99%

Global three‐dimensional MHD simulation of a space weather event: CME formation, interplanetary propagation, and interaction with the magnetosphere

Groth

Zeeuw²,

Gombosi³

et al. 2000

J. Geophys. Res.

263

255

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Abstract. A parallel adaptive mesh refinement (AMR) finite-volume scheme for predictingideal MHD flows is used to simulate the initiation, structure, and evolution of a coronal mass ejection (CME) and its interaction with the magnetosphere-ionosphere system. The simulated CME is driven by a local plasma density enhancement on the solar surface with the background initial state of the corona and solar wind represented by a newly devised "steady state" solution. The initial solution has been constructed to provide a reasonable description of the time-averaged solar wind for conditions near solar minimum: (1) the computed magnetic field near the Sun possesses high-latitude polar coronal holes, closed magnetic field flux tubes at low latitudes, and a helmet streamer structure with a neutral line and current sheet; (2) the Archimedean spiral topology of the interplanetary magnetic field is reproduced; (3) the observed two-state nature of the solar wind is also reproduced with the simulation yielding fast and slow solar wind streams at high and low latitudes, respectively; and (4) the predicted solar wind plasma properties at 1 AU are consistent with observations. Starting with the generation of a CME at the Sun, the simulation follows the evolution of the solar wind disturbance as it evolves into a magnetic cloud and travels through interplanetary space and subsequently interacts with the terrestrial magnetosphere-ionosphere system. The density-driven CME exhibits a two-step release process, with the front of the CME rapidly accelerating following the disruption of the near-Sun closed magnetic field line structure and then moving at a nearly constant speed of •560 km/s through interplanetary space. The CME also produces a large magnetic cloud (> 100/•s across) characterized by a magnetic field that smoothly rotates northward and then back again over a period of •2 days at 1 AU. The cloud does not contain a sustained period with a strong southward component of the magnetic field, and, as a consequence, the simulated CME is somewhat ineffective in generating strong geo-magnetic activity at Earth. Nevertheless, the simulation results illustrate the potential, as well as current limitations, of the MHD-based space weather model for enhancing the understanding of coronal physics, solar wind plasma processes, magnetospheric physics, and space weather phenomena. Such models will provide the foundation for future, more comprehensive space weather prediction tools.

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confidence: 99%

Global three‐dimensional MHD simulation of a space weather event: CME formation, interplanetary propagation, and interaction with the magnetosphere

Groth

Zeeuw²,

Gombosi³

et al. 2000

J. Geophys. Res.

263

255

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“…Inner zone flux changes are not followed because of the L=2.3 inner boundary of the MHD simulation. Electric and magnetic fields are mapped to the ionosphere assuming Hall and Pederson conductivities which evolve in time with magnetic fieldaligned currents, simulating auroral ionization (Fedder et al, 1995). No plasmasphere was included for these long time scale runs, which require an evolving plasmasphere, in contrast to simulations of the rapid March 24, 1991 injection event, where the plasmasphere was characterized by initial planetary magnetic activity in dex Kp (Moore et al, 1987).…”

Section: Simulationsmentioning

confidence: 99%

Radiation Belt Electron Acceleration by ULF Wave Drift Resonance: Simulation of 1997 and 1998 Storms

Hudson

Elkington

Lyon

et al. 2013

Geophysical Monograph Series

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Pc 5 ULF waves are seen concurrently with the rise in radiation belt fluxes associated with CME-magnetic cloud events. Four such geomagnetic storm periods in 1997 and 1998, 10-11 January and 14-15 May, 1997; 1-4 May and 26-28 August, 1998, have been simulated with a 3D global MHD code driven by Ll-measured solar wind parameters. The field output has been used to advance electron guiding center trajectories in the equatorial plane. The time series has also been analyzed for ULF wave mode structure. Toroidal field line resonances with low azimuthal mode number and frequencies com mensurate with the electron drift period are identified in the radial electric field component, along with enhanced power in the poloidal (azimuthal) elec tric field component. The simulated time scale for inward radial transport of electrons in the several hundred keV to MeV energy range, from geosyn chronous orbit to L=3-4, varies with the level of ULF wave power and overall energy input to the magnetosphere. Of the four events studied, the May 1998 storm period was most geoeffective and the January 1997 least so, in terms of simulated radial transport and energization of electrons. This transport rate is consistent with the level of ULF waves excited in the simulations, and the proposed drift resonant acceleration mechanism.

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“…The Lyon-FedderMobarry (LFM) simulation model [Fedder et al, 1995;Lyon et al, 1998] has been used to examine several substorm events, and the results have shown that the code reproduces well the observed main sequence of events during substorms. The magnetospheric output obtained from simulations driven by actual solar wind data is then used as input into the ionosphere.…”

Section: Introductionmentioning

confidence: 99%

Modeling ionospheric absorption modified by anomalous heating during substorms

Milikh

Dimant

Shao

et al. 2001

Geophysical Research Letters

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Abstract. Riometers monitor the changes in ionospheric conductivity by measuring the absorption of very high frequency radio noise of galactic origin passing through the ionosphere. In this Letter the absorption of radio signals by a thin layer of ionospheric plasma, produced by ionization due to energetic precipitating electrons, is modeled by taking into account strong turbulent heating caused by instabilities. The precipitating electron population is obtained from a global MHD simulation of the magnetosphere, along with the electric fields which excite the Farley-Buneman instability and lead to turbulent electron heating. A comparison, the first of its kind, of the data from polar and sub-auroral riometers for the magnetic cloud event of January 10, 1997 shows good agreement. The ionospheric conductance modified by turbulent electron heating can be used to improve the magnetosphereionosphere coupling in the current global MHD models.

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Global numerical simulation of the growth phase and the expansion onset for a substorm observed by Viking

Cited by 154 publications

References 17 publications

Global three‐dimensional MHD simulation of a space weather event: CME formation, interplanetary propagation, and interaction with the magnetosphere

Global three‐dimensional MHD simulation of a space weather event: CME formation, interplanetary propagation, and interaction with the magnetosphere

Radiation Belt Electron Acceleration by ULF Wave Drift Resonance: Simulation of 1997 and 1998 Storms

Modeling ionospheric absorption modified by anomalous heating during substorms

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