標題: Titlebook: Advances in Solar Research at Eclipses from Ground and from Space; Proceedings of the N Jean-Paul Zahn,Magda Stavinschi Conference proceedi [打印本頁] 作者: STRI 時間: 2025-3-21 19:50
書目名稱Advances in Solar Research at Eclipses from Ground and from Space影響因子(影響力)
書目名稱Advances in Solar Research at Eclipses from Ground and from Space影響因子(影響力)學科排名
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書目名稱Advances in Solar Research at Eclipses from Ground and from Space被引頻次學科排名
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書目名稱Advances in Solar Research at Eclipses from Ground and from Space年度引用學科排名
書目名稱Advances in Solar Research at Eclipses from Ground and from Space讀者反饋
書目名稱Advances in Solar Research at Eclipses from Ground and from Space讀者反饋學科排名
作者: 最高峰 時間: 2025-3-21 23:50 作者: notification 時間: 2025-3-22 04:07
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作者: CLEAR 時間: 2025-3-22 07:15
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”作者: 煞費苦心 時間: 2025-3-22 12:13 作者: paragon 時間: 2025-3-22 14:13 作者: 古代 時間: 2025-3-22 19:26 作者: resilience 時間: 2025-3-22 23:23
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作者: remission 時間: 2025-3-23 04:35 作者: 主講人 時間: 2025-3-23 08:11 作者: 領巾 時間: 2025-3-23 11:39 作者: PIZZA 時間: 2025-3-23 15:07 作者: 上下連貫 時間: 2025-3-23 18:37 作者: Pericarditis 時間: 2025-3-24 01:33
978-0-7923-6624-9Springer Science+Business Media Dordrecht 2000作者: 類型 時間: 2025-3-24 04:21 作者: Interlocking 時間: 2025-3-24 08:01
Bo Jiang,Xuejun Xu,Junchen Yang,Tian WangThis chapter briefly describes:作者: 系列 時間: 2025-3-24 13:09 作者: ADAGE 時間: 2025-3-24 16:27
Eclipses from the Standpoint of Celestial Mechanics,This chapter briefly describes:作者: 箴言 時間: 2025-3-24 21:18 作者: 英寸 時間: 2025-3-25 00:24
Advances in Solar Research at Eclipses from Ground and from Space978-94-011-4325-7Series ISSN 1389-2185 作者: Decibel 時間: 2025-3-25 04:37 作者: EVEN 時間: 2025-3-25 07:50
Zhi-bing Fu,Qing-kui Chen,Ming-ming Wanga, observed at the ground only during total solar eclipses a long time ago, has been observed with special coronographs since the ‘30s. However, the last three decades, beginning with OSO 7 and Skylab space missions, contributed enormously to our present knowledge of the solar corona. Today the coro作者: 詢問 時間: 2025-3-25 13:11
Jianqing Weng,Songzhi Su,Xiaoliang Fan 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作者: choroid 時間: 2025-3-25 18:43
Wenju Chen,Kun Guo,Yuzhong Chen 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”作者: curriculum 時間: 2025-3-25 19:59 作者: 少量 時間: 2025-3-26 02:21 作者: diathermy 時間: 2025-3-26 07:10
https://doi.org/10.1007/978-981-99-9640-7l approach that captures the complicated dynamical interaction between plasma and magnetic fields. These equations are therefore widely used for investigating the dynamical processes that takes place in the solar atmosphere. The MHD equations can also be used to provide information about the field l作者: 滔滔不絕地講 時間: 2025-3-26 11:02
https://doi.org/10.1007/978-981-99-9640-7ocal 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作者: 遠地點 時間: 2025-3-26 13:59
Shuai Liu,Zi-Jia Wang,Zong-Gan Chenr. While most of stellar atmospheres are simply modelled as one-dimensional (1D) plane-parallel or spherically-symmetrical layer, the solar atmosphere must generally be resolved into various brightness components which also exhibit quite different behaviour. Therefore, a single solar atmospheric mod作者: chandel 時間: 2025-3-26 19:14
https://doi.org/10.1007/978-981-99-9637-7e interior and, first of all, to explain the source of the energy radiated by the Sun. Already sir Arthur Eddington in his . published in 1926 presents the hypothesis that the energy is liberated in building up helium nucleus from four protons, as most plausible explanation. By early 1940ies, mostly作者: CRUMB 時間: 2025-3-26 21:58 作者: Constitution 時間: 2025-3-27 01:36
Yajing Li,Jianbo Xu,Guozheng Feng,Wei Jianhanges in surface emissivity, i.e. the reduced cooling in spots and enhanced emission by small scale magnetic fields, are the most effective mechanisms and account for most of the observed variation. Helioseismology will soon be able to test the consequences of changes in surface emissivity, and dis作者: GRAZE 時間: 2025-3-27 05:56 作者: 偏離 時間: 2025-3-27 13:04
Modeling the Evolution of Solar Magnetic Fields,, heating profiles. This paper gives a review of magnetic reconnection, the basic idea behind magnetic field extrapolation, and the problems related to using temperature profiles for determining the underlying heating profile. A full understanding and utilisation of all of these disciplines within s作者: capillaries 時間: 2025-3-27 13:36 作者: 生存環(huán)境 時間: 2025-3-27 21:28 作者: 殘忍 時間: 2025-3-28 01:58 作者: 借喻 時間: 2025-3-28 05:36
Conference proceedings 2000e 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.作者: Blood-Clot 時間: 2025-3-28 06:38
1389-2185 ecently 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.978-0-7923-6624-9978-94-011-4325-7Series ISSN 1389-2185 作者: 僵硬 時間: 2025-3-28 13:51 作者: miniature 時間: 2025-3-28 17:06 作者: 廢除 時間: 2025-3-28 18:46 作者: Disk199 時間: 2025-3-29 02:29 作者: indoctrinate 時間: 2025-3-29 06:04
Observing the Solar Magnetic Field,powerful for low-resolution magnetic diagnostics based on analysis of Hanle effect in prominences and the emission line corona. Employment of a new generation large-aperture reflecting coronagraph allows to expect advances in high-resolution magnetic observations of prominence and coronal structures.作者: animated 時間: 2025-3-29 10:18
Solar Activity,activity indices and activity mapping, the 11-, 22- and 100-year solar activity cycles, and their effect on the quiet sun, with solar variability. We finish with a few comments on the solar-stellar relation.作者: NADIR 時間: 2025-3-29 11:48 作者: 赦免 時間: 2025-3-29 18:09 作者: GRAZE 時間: 2025-3-29 22:52 作者: Lacunar-Stroke 時間: 2025-3-30 00:55
Wenan Tan,Zhejun Liang,Jin Liu,Kai Dingd in the last twenty years, which permits to probe directly the solar interior by means of acoustic waves, and this had a tremendous impact on solar physics because it provides tight observational constraints on our models. We shall illustrate this here by a few examples of recent advances in modeling the Sun.作者: intention 時間: 2025-3-30 06:24
Heliospheric Extent of the Coronal Phenomena,na is watched both from ground and from space. The solar space missions Yohkoh and SOHO are registering coronal phenomena in the X and UV radiations in the ecliptic plane, while Ulysses is crossing over the polar solar region (at an angle of about 87° with the ecliptic plan).
