By Abraham C.-L. Chian (auth.), A. C.-L. Chian, I. H. Cairns, S. B. Gabriel, J. P. Goedbloed, T. Hada, M. Leubner, L. Nocera, R. Stening, F. Toffoletto, C. Uberoi, J. A. Valdivia, U. Villante, C.-C. Wu, Y. Yan (eds.)
Advances in area setting learn - quantity I includes the lawsuits of 2 foreign workshops, the area area setting discussion board (WSEF2002) and the excessive functionality Computing in house setting learn (HPC2002), geared up through the area Institute for area atmosphere examine (WISER) from 22 July to two August 2002 in Adelaide, Australia.
The articles during this quantity overview the cutting-edge of the theoretical, computational and observational stories of the actual procedures of Sun-Earth connections and house surroundings. They disguise six topical parts: Sun/Heliosphere, Magnetosphere/Bow surprise, Ionosphere/Atmosphere, area Weather/Space weather, house Plasma Physics/Astrophysics, and Complex/Intelligent structures.
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Additional info for Advances in Space Environment Research: Volume I
Kaiser, M. , Howard, R. A. and Bougeret, J. : 2001a, ‘Characteristics of Coronal Mass Ejectrions Associated with Long-Wavelength Type II Radio Bursts’, J. Geophys. Res. 106, 29219 – 29229. , Kaiser, M. , Howard, R. A. and Bougeret, J. ’, Astrophys. J. 548, L91 – 94. Knock, S. , Cairns, I. , Robinson, P. A. : 2001, ‘Theory of Type II Radio Emission from the Foreshock of an Interplanetary Shock’, J. Geophys. Res. 106, 25041 – 25051. Knock, S. , Cairns, I. , Robinson, P. A. : 2003, ‘Theoretically predicted properties of Type II radio Emission from an Interplanetary Foreshock’, J.
2. Basic Theory Consider the global shock or a localized ripple thereon (cf. , 1999). Important shock/ripple parameters are (Figure 1): U = |Vsh − vsw | is the shock’s speed relative to the plasma, where Vsh and vsw are the (aligned) shock velocity and solar wind velocity, respectively, B1 is the upstream magnetic ﬁeld vector, θbu the angle between Vsh and B1 , and b is the shock’s curvature parameter deﬁned by X = bY 2 . Then b = Rc−1 , where Rc is the radius of curvature at the shock’s nose. The important plasma properties are the electron and ion temperatures Te and Ti and the parameter κ of the incoming, gyrotropic, generalized-Lorentzian electron distribution, deﬁned by fκ (v , v⊥ ) = v 2 + v⊥2 (κ + 1) −3/2 −3 π Ve 1+ (κ) Ve2 −(κ+1) (1) √ where Ve = kB Te /me is the electron thermal speed.
1959, ‘Hydromagnetic Theory of Geomagnetic Storms’, J. Geophys. Res. 64, 2239 – 2252. Feldstein, Y. I. : 1999, ‘Dynamics of the Auroral Elecrtojets and Their Mapping to the Magnetosphere’, Ragiation Measurements 30, N 5, 579 – 587. Iijima, T. and Potemra, T. : 1976, ‘The Amplitude Distribution of Field-Aligned Currents at Northern High Latitudes Observed by Triad’, J. Geophys. Res. 81, 2165 – 2174. : 2000, ‘Magnetosheath Conditions and Magnetopause Structure for High Magnetic Shear’, Phys. and Chem.