MHD Simulation of the “Geoeffectiveness” of Interplanetary Disturbances

Dryer, M.; Smith, Z.; Wu, S. T.; Han, S. M.; Yeh, Tom

doi:10.1007/978-94-009-4722-1_15

Cited by 10 publications

(2 citation statements)

References 24 publications

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“…The approach of Nakagawa and Wellck (1973) and Hirshberg, Nakagawa, and Wellck (1974) was pursued in the 2-D, time-dependent magnetic approach by Han (1976, 1983) and Dryer et al (1986). The latter authors first produced a corotating stream by using an input pulse at 18 R o in which the velocity increased from 250 km s-1 to 320 km s-1 and which had the form of a symmetric, 35 ~ wide trapezoid in azimuth.…”

Section: Introductionmentioning

confidence: 99%

Numerical simulations of high-speed solar wind streams within 1 AU and their signatures at 1 AU

Smith

Dryer

1991

Sol Phys

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A parametric study of the evolution within, and signatures at, 1 AU of high-speed streams is performed with the use of a MHD, 2 89 time-dependent model. This study is an extension of an earlier one by Smith and Dryer (1990) who examined the ecliptic plane consequences of relatively short-duration, energetic solar disturbances. The present study examines both the erupting and corotating parts of longduration, high-speed streams characteristic of coronal hole flows. By examining the variation of the simulated plasma velocity, density, temperature, and magnetic field at 1 AU, as well as the location of the solar coronal hole sources relative to the observer at 1 AU, we are able to provide some insight into the identification of the solar sources of interplanetary disturbances. We present and discuss two definitions for angle locating the solar source of interplanetary disturbances at 1 AU.We apply our results to the suggestion by Hewish (1988) that low-latitude coronal holes are suitably positioned to be the sources of maj or geomagnetic storms when the holes are in the eastern half of the solar hemisphere at the time of the commencement of the storm. Our results indicate that, for these cases, the streams emanating from within the hole must be very fast, greater than 1000 km s -1, or very wide, greater than 60 ~ at the inner boundary of 18 solar radii in our simulation.

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Section: Introductionmentioning

confidence: 99%

Numerical simulations of high-speed solar wind streams within 1 AU and their signatures at 1 AU

Smith

Dryer

1991

Sol Phys

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“…A multi-spacecraft test (using Prognoz 1 and Pioneer 9 data for comparison) was performed with the 2D model (D'Uston, 1981) for the August 1972 events. The 2-1/2D model has been tested (V and IBI only) against ISEEdata during the August 1979 epoch (STIP Interval VII) with success in predicting the major structures and amplitudes (Dryer et al, 1986a) but with some timing offsets.…”

Section: Introductionmentioning

confidence: 99%

Multi-spacecraft testing of time-dependent interplanetary MHD models for operational forecasting of geomagnetic storms

Dryer

Smith

1989

Earth Moon Planet

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An MHD 2-1/2D, time-dependent model is used, together with observations of six solar flares during 3-7 February 1986, to 'demonstrate global, large-scale, compound disturbances in the solar wind over a wide range of heliolongitudes. This scenario is one that is likely to occur many times during the cruise, possibly even encounter, phases of the Multi-Comet Mission. It is suggested that a model such as this one should be tested with multi-spacecraft data (such as the MCM and Earth-based probes) with several goals in view: (1) utility of the model for operational real-time forecasting of geomagnetic storms, and (2) scientific interpretation of certain forms of cometary activities and their possible association with solar-generated activity.

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Computation of interplanetary hydromagnetic disturbances in a synoptic domain

Yeh

1987

Commun. appl. numer. methods

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SUMMARYThe constraints on initial and boundary data for magnetic solenoidality are implemented for MHD computation of interplanetary disturbances. The domain of computation is the entire ecliptic plane outside the solar equator. It is a synoptic domain, without cuts as artificial boundaries. The radial co-ordinate is stretched so that grid points constitute equilateral meshes, to attain the same degree of accuracy in the finite difference approximations for spatial derivatives in orthogonal directions.

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MHD Simulation of the “Geoeffectiveness” of Interplanetary Disturbances

Cited by 10 publications

References 24 publications

Numerical simulations of high-speed solar wind streams within 1 AU and their signatures at 1 AU

Numerical simulations of high-speed solar wind streams within 1 AU and their signatures at 1 AU

Multi-spacecraft testing of time-dependent interplanetary MHD models for operational forecasting of geomagnetic storms

Computation of interplanetary hydromagnetic disturbances in a synoptic domain

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