| 書目名稱 | The Origin and Dynamics of Solar Magnetism |
| 編輯 | M. J. Thompson,A. Balogh,J.-P. Zahn |
| 視頻video | http://file.papertrans.cn/916/915329/915329.mp4 |
| 概述 | Treats the topics of solar variability and how the solar dynamo works in great detail.Dynamics and evolution of magnetic fields that drive solar activity are treated in a very comprehensive way |
| 叢書名稱 | Space Sciences Series of ISSI |
| 圖書封面 |  |
| 描述 | Starting in 1995 numerical modeling of the Earth’s dynamo has ourished with remarkable success. Direct numerical simulation of convection-driven MHD- ow in a rotating spherical shell show magnetic elds that resemble the geomagnetic eld in many respects: they are dominated by the axial dipole of approximately the right strength, they show spatial power spectra similar to that of Earth, and the magnetic eld morphology and the temporal var- tion of the eld resembles that of the geomagnetic eld (Christensen and Wicht 2007). Some models show stochastic dipole reversals whose details agree with what has been inferred from paleomagnetic data (Glatzmaier and Roberts 1995; Kutzner and Christensen 2002; Wicht 2005). While these models represent direct numerical simulations of the fundamental MHD equations without parameterized induction effects, they do not match actual pla- tary conditions in a number of respects. Speci cally, they rotate too slowly, are much less turbulent, and use a viscosity and thermal diffusivity that is far too large in comparison to magnetic diffusivity. Because of these discrepancies, the success of geodynamo models may seem surprising. In order to better understand |
| 出版日期 | Book 20091st edition |
| 關(guān)鍵詞 | Corona; Heliosphere; Photosphere; Planet; Sunspot; dynamics solar cycle; helioseismology; helioseismology s |
| 版次 | 1 |
| doi | https://doi.org/10.1007/978-1-4419-0239-9 |
| isbn_softcover | 978-1-4614-1710-1 |
| isbn_ebook | 978-1-4419-0239-9Series ISSN 1385-7525 |
| issn_series | 1385-7525 |
| copyright | Springer-Verlag New York 2009 |
|Archiver|手機版|小黑屋|
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