By Wing-huen Ip
"Advances in Geosciences" is the results of a concerted attempt in bringing the most recent effects and making plans actions on the topic of earth and house technology in Asia and the foreign area. the amount editors are all prime scientists of their examine fields protecting 5 sections: strong Earth (SE), sunlight Terrestrial (ST), Planetary technology (PS), Hydrological technological know-how (HS), and Oceans and Atmospheres (OA). the most goal is to focus on the medical concerns necessary to the research of earthquakes, tsunamis, weather switch, drought, flood, typhoons, house weathers, and planetary exploration.
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Additional resources for Advanced in Geoscience, V3: Planetary Science(Ps) (2006)(en)(416s)
5 RM radial distance and for two diﬀerent temperatures (30 eV and 1 keV) of the initial Maxwellian distribution (adapted from Ref. 17). dipolarization. Here, the test particles were initialized with 10 eV energy and 90◦ pitch angle at diﬀerent locations (separated by equidistant steps of 500 km) along the ﬁeld line. , Ref. 20) is clearly noticeable in these panels that display a rapid inward injection of the electrons. Also, because of the low-energy character of the particles (up to a few hundreds of eV after dipolarization), no signiﬁcant drift in the Y -direction can be seen in the bottom left panel.
103 (1998) 9113–9119. 40. W. H. Smyth and M. L. Marconi, Icarus 441 (1995) 839–864. 41. B. V. Yakshinskiy, T. E. Madey and V. N. Ageev, Surf. Rev. Let. 7 (2000) 75–87. 42. H. Schleicher, G. Wiedemann, H. W¨ ohl, T. Berkefeld and D. Soltau, A&A 425 (2004) 1119–1124. 43. A. L. Sprague, Icarus 84 (1990) 93–105. 44. N. Yan, F. Leblanc and E. Chasseﬁ`ere, Icarus (2006). 45. R. E. Johnson, Surface boundary layer atmospheres, Chapter in Atmospheres in the Solar System: Comparative Aeronomy Geophysical Monograph 130 (2002) 203–219.
23). At Mercury, one may expect this non-adiabatic heating to aﬀect plasma sheet H+ populations due to the short-time scale of magnetic transitions. This is illustrated in Fig. 5 that shows model H+ trajectories in a 5-second dipolarization identical to that in Fig. 4. Here, test protons were initialized with 100 eV energy and 90◦ pitch angle at diﬀerent (grey-coded) positions along the dipolarizing ﬁeld line. It is clearly apparent from Fig. 5 that most of the test H+ are subjected to prominent magnetic moment enhancement and energization (up to several tens of keV), with the exception of the ions initialized close to the planet surface that have small Larmor radii and small gyration periods.