Physics – Geophysics
Scientific paper
Oct 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984ap%26ss.105..187d&link_type=abstract
Astrophysics and Space Science (ISSN 0004-640X), vol. 105, no. 1, Oct. 1984, p. 187-208.
Physics
Geophysics
22
Interplanetary Magnetic Fields, Magnetic Disturbances, Magnetohydrodynamics, Shock Wave Propagation, Solar Terrestrial Interactions, Solar Wind Velocity, Canonical Forms, Forecasting, Geophysics, Ionospheric Disturbances, Magnetic Storms, Magnetospheric Instability, Solar Flares, Two Dimensional Models
Scientific paper
A time-dependent, nonplanar, two-dimensional magnetohydrodynamic computer model is used to simulate a series, separately examined, of solar flare-generated shock waves and their subsequent disturbances in interplanetary space between the sun and the earth's magnetosphere. The 'canonical' or ansatz series of shock waves include initial velocities near the sun over the range 500 to 3500 km/s. The ambient solar wind, through which they propagate, is taken to be a steady state homogeneous plasma (that is, independent of heliolongitude) with a representative set of plasma and magnetic field parameters. Complete sets of solar wind plasma and magnetic field parameters are presented and discussed. Particular attention is addressed to the MHD model's ability to address fundamental operational questions vis-a-vis the long-range forecasting of geomagnetic disturbances. These questions are: (1) will a disturbance (such as the present canonical series of solar flare shock waves) produce a magnetospheric and ionospheric disturbance, and, if so, (2) when will it start, (3) how severe will it be, and (4) how long will it last? The model's output is used to compute various solar wind indices of current interest as a demonstration of the model's potential for providing 'answers' to these questions.
Dryer Murray
Gislason G.
Han Ming Sheng
Shea Margaret Ann
Smart Don Frederick
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