| 書目名稱 | Solar Photosphere: Structure, Convection, and Magnetic Fields | | 副標(biāo)題 | Proceedings of the 1 | | 編輯 | J. O. Stenflo | | 視頻video | http://file.papertrans.cn/872/871408/871408.mp4 | | 叢書名稱 | International Astronomical Union Symposia | | 圖書封面 |  | | 描述 | Solar and stellar photospheres constitute the layers most accessible to observations, forming the interface between the interior and the outside of the stars. The solar atmosphere is a rich physics laboratory, in which the whole spectrum of radiative, dynamical, and magnetic processes that tranfer energy into space can be observed. As the fundamental processes take place on very small spatial scales, we need high· resolution observations to explore them. On the other hand the small-scale processes act together to form global properties of the sun, which have their origins in the solar interior. The rapid advances in observational techniques and theoreticallllodelling over the past decade made it very timely to bring together scientists from east and west to the first lAU Symposium on this topic. The physics of the photosphere involves complicated interactions between magnetic fields, convection, waves, and radiation. During the past decade our understanding of these gener- ally small-scale structures and processes has been dramatically advanced. New instrumen- tations, on ground and in space, have given us new means to study the granular convection. Diagnostic methods in Stokes pol | | 出版日期 | Conference proceedings 1990 | | 關(guān)鍵詞 | Main sequence; Photosphere; Sunspot; helioseismology; solar | | 版次 | 1 | | doi | https://doi.org/10.1007/978-94-009-1061-4 | | isbn_softcover | 978-0-7923-0530-9 | | isbn_ebook | 978-94-009-1061-4Series ISSN 1743-9213 Series E-ISSN 2352-2186 | | issn_series | 1743-9213 | | copyright | International Astronomical Union 1990 |
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書目名稱Solar Photosphere: Structure, Convection, and Magnetic Fields影響因子(影響力)
書目名稱Solar Photosphere: Structure, Convection, and Magnetic Fields影響因子(影響力)學(xué)科排名
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書目名稱Solar Photosphere: Structure, Convection, and Magnetic Fields被引頻次
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