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  Planetary Magnetic Fields and Dynamos
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アイテムのパーマリンク: https://hdl.handle.net/21.11116/0000-0006-5B43-9 版のパーマリンク: https://hdl.handle.net/21.11116/0000-0006-9F49-6
資料種別: 百科事典への寄稿

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 作成者:
Christensen, Ulrich R.1, 著者           
所属:
1Department Planets and Comets, Max Planck Institute for Solar System Research, Max Planck Society, ou_1832288              

内容説明

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キーワード: planetary core, magnetic field, magnetic dipole, dynamo, convection, magnetohydrodynamics
 要旨: Since 1973 space missions carrying vector magnetometers have shown that most, but not all, solar system planets have a global magnetic field of internal origin. They have also revealed a surprising diversity in terms of field strength and morphology. While Jupiter’s field, like that of Earth, is dominated by a dipole moderately tilted relative to the planet’s spin axis, the fields of Uranus and Neptune are multipole-dominated, whereas those of Saturn and Mercury are highly symmetric relative to the rotation axis. Planetary magnetism originates from a dynamo process, which requires a fluid and electrically conducting region in the interior with sufficiently rapid and complex flow. The magnetic fields are of interest for three reasons: (i) they provide ground truth for dynamo theory, (ii) the magnetic field controls how the planet interacts with its space environment, for example, the solar wind, and (iii) the existence or nonexistence and the properties of the field enable us to draw inferences on the constitution, dynamics, and thermal evolution of the planet’s interior. Numerical simulations of the geodynamo, in which convective flow in a rapidly rotating spherical shell representing the outer liquid iron core of the Earth leads to induction of electric currents, have successfully reproduced many observed properties of the geomagnetic field. They have also provided guidelines on the factors controlling magnetic field strength and morphology. For numerical reasons the simulations must employ viscosities far greater than those inside planets and it is debatable whether they capture the correct physics of planetary dynamo processes. Nonetheless, such models have been adapted to test concepts for explaining magnetic field properties of other planets. For example, they show that a stable stratified conducting layer above the dynamo region is a plausible cause for the strongly axisymmetric magnetic fields of Mercury or Saturn.

資料詳細

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言語: eng - English
 日付: 2019
 出版の状態: オンラインで出版済み
 ページ: -
 出版情報: -
 目次: -
 査読: -
 識別子(DOI, ISBNなど): DOI: 10.1093/acrefore/9780190647926.013.31
 学位: -

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出版物 1

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出版物名: Oxford Research Encyclopedia: Planetary Science
種別: 百科事典
 著者・編者:
Oxford University Press, 編集者              
所属:
-
出版社, 出版地: Oxford : Oxford Univ. Press
ページ: - 巻号: - 通巻号: - 開始・終了ページ: - 識別子(ISBN, ISSN, DOIなど): その他: https://oxfordre.com/