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Titlebook: Advances in Solar Research at Eclipses from Ground and from Space; Proceedings of the N Jean-Paul Zahn,Magda Stavinschi Conference proceedi

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發(fā)表于 2025-3-21 19:50:27 | 只看該作者 |倒序?yàn)g覽 |閱讀模式
期刊全稱(chēng)Advances in Solar Research at Eclipses from Ground and from Space
期刊簡(jiǎn)稱(chēng)Proceedings of the N
影響因子2023Jean-Paul Zahn,Magda Stavinschi
視頻videohttp://file.papertrans.cn/150/149802/149802.mp4
學(xué)科分類(lèi)Nato Science Series C:
圖書(shū)封面Titlebook: Advances in Solar Research at Eclipses from Ground and from Space; Proceedings of the N Jean-Paul Zahn,Magda Stavinschi Conference proceedi
影響因子The aim of this Advanced Study Institute was to give an account on the most recent results obtained in solar research. Bucharest was chosen to host it, because the capital city of Romania was located right in the middle of the totality path of the last eclipse of the millennium, on 11th August 1999; furthermore the phenomenon was close to reach there its longest duration: 2m 23s. Such a total eclipse is not only a very spectacular event which draws the crowds: to astronomers, solar eclipses still offer the best conditions for observing the lower part of the corona. The Sun plays a crucial role in our very existence. It was responsible for the formation of the Earth, and rendered this planet fit to host living beings, providing the right amount of heat, and this for a long enough span of time. Quite understandably, it has always been a prime target of human curiosity, and more recently one of scientific investigation. During the last century, it was realized that the Sun is a star like billions of others; we learned since that it draws its energy from the nuclear fusion of hydrogen, and we are now able to estimate its age and life expectancy.
Pindex Conference proceedings 2000
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The Solar Corona: White Light Polarization and Modelling of the Large Scale Electron Density Distri loops and of streamers, extending up to several solar radii. The corona is separated from the chromosphere by a narrow transition region with very high temperature gradients. In this very thin layer, the temperature increases from about 10 000 K in the chromosphere up to millions K in the corona. T
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Observing the Solar Magnetic Field, than the line width. This corresponds to magnetic observations of chromosphere, prominences and the corona requiring more advanced technique as compared with the photosphere. Direct and indirect methods of magnetic researches in the upper solar atmosphere are briefly reviewed. The “signal-to-noise”
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Non-LTE Radiation Processes: Application to the Solar Corona,ocal thermodynamical equilibrium (NLTE), without appealing to any previous knowledge except a few basics of physics and spectroscopy. After recalling elementary notions of radiation transfer, the chapter is focussed on the computation of the level populations, the source function, the ionization sta
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