Download Earth's Low-Latitude Boundary Layer by W.J. Heikkila PDF

By W.J. Heikkila

Published by way of the yank Geophysical Union as a part of the Geophysical Monograph Series.

We think the reader of this preface status on the AGU book shop puzzling over if the tome in hand is worthy procuring. the answer's “no”, apart from convinced trifling exceptions. those that desire to find out about the intriguing pioneering years of LLBL study should purchase the e-book for Tim Eastman's first-class historic evaluate, our starting bankruptcy. whilst did the time period “LLBL” first input the sphere? Eastman will let you know, and lots more and plenty else besides.


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6. Comparison with numerical simulation. In Plate 1, various qualitative features of the analytical model are verified by comparison with results from a nu­ merical simulation of unmagnetized solar-wind flow past the magnetosphere, using results from the Integrated Space Weather Prediction Model (ISM) simulation code (see Sonnerup et al. [2001] for details). Plate l a shows a color-coded m a p of flow velocity v averaged over one hour, in the equatorial plane: tailward flow regions are blue, sunward flows are tan.

Lysak, A two-dimensional simu­ lation of the Kelvin-Helmholtz instability with magnetic shear, J. Geophys. , 104, 25,097, 1999. Kelley, M. C , The Earth's Ionosphere, Plasma Physics and Electrodynamics, p. , San Diego, 1989. , Parallel electric fields, Planet. , 21, 741, 1973. T. Russell, J. T. Gosling, and M. F. Thomsen, ISEE observations of low-latitude boundary layer for northward interplanetary magnetic field: Implications for cusp reconnection, J. Geophys. , 101, 27,239, 1996. Lee, L. C , R.

In the limit M = 0 it would become a delta function distri­ bution in latitude, with sufficient net current to satisfy hot = 2 E p $ p c x x 2 t e e to e e r 0. i i i I 1. i i i I i i 2. i I i i i 3. I 4. Y F i g u r e 4. Steady LLBL flow with field-aligned potential drops for various values of the Hartmann number, M = 2, 5, 10, 20, 50, and 200. Panel(a): Normalized equatorial electric field (or, equivalently, plasma velocity) versus Y = y/X . Panel(b): Ionospheric electric field, normalized by the same electric field as in (a), versus Y = y /X .

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