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Titlebook: Solar System Magnetic Fields; E. R. Priest Book 1985 D. Reidel Publishing Company, Dordrecht, Holland 1985 Corona.Planet.Solar.Solar Syste

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发表于 2025-3-21 18:50:16 | 显示全部楼层 |阅读模式
书目名称Solar System Magnetic Fields
编辑E. R. Priest
视频video
丛书名称Geophysics and Astrophysics Monographs
图书封面Titlebook: Solar System Magnetic Fields;  E. R. Priest Book 1985 D. Reidel Publishing Company, Dordrecht, Holland 1985 Corona.Planet.Solar.Solar Syste
描述In September 1984 a Summer School on Solar System Plasmas was held at Imperial College with the support of the Science and Engineering Research Council. An excellent group of lecturers was assembled to give a series of basic talks on the various aspects of the subject, aimed at Ph. D. students or researchers from related areas wanting to learn about the plasma physics of the solar system. The students were so appreciative of the lectures that it was decided to write them up as the present book. Traditionally, different areas of solar system science, such as solar and magnetospheric physics, have been studied by separate communities with little contact. However, it has become clear that many common themes cut right across these distinct topics, such as magnetohydrodynamic instabilities and waves, magnetic reconnect ion , convection, dynamo activity and particle acceleration. The plasma parameters may well be quite different in the Sun‘s atmosphere, a cometary tailor Jupiter‘s magnetosphere, but many of the basic processes are similar and it is by studying them in different environments that we come to understand them more deeply. Furthermore, direct in situ measurements of plasma pr
出版日期Book 1985
关键词Corona; Planet; Solar; Solar System; Solar flare; Solar wind; Sun; Sunspot
版次1
doihttps://doi.org/10.1007/978-94-009-5482-3
isbn_softcover978-90-277-2138-9
isbn_ebook978-94-009-5482-3
copyrightD. Reidel Publishing Company, Dordrecht, Holland 1985
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Magnetoconvection,gnetic field; and, third, the structure of the large-scale magnetic field in the sun (which leads on to the discussion of dynamo theory in Chapter 7). Various aspects of magnetoconvection have been considered in a number of recent reviews (Priest, 1982; Proctor and Weiss, 1982; Galloway, 1984; Nordl
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Book 1985rameters may well be quite different in the Sun‘s atmosphere, a cometary tailor Jupiter‘s magnetosphere, but many of the basic processes are similar and it is by studying them in different environments that we come to understand them more deeply. Furthermore, direct in situ measurements of plasma pr
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