Coronal structure and brightness profile of the total solar eclipse on August 1,2008  

作　　者：ZHAO HaiBin LIN QiSheng CHEN YiPing JIN Sheng GUAN ZhenBiao HU ZhongWei 

机构地区：[1]Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210008, China [2]National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China [3]Lulin Observatory, Taoyuan 32054, Taiwan, China [4]Department of Astronomy, Nanjing University, Nanjing 210008, China

出　　处：《Chinese Science Bulletin》2009年第16期2905-2908,共4页

基　　金：Supported by the National Natural Science Foundation of China (Grant Nos. 10503013, 10778637);Minor Planet Foundation of Purple Mountain Observatory, Chinese Academy of Sciences

摘　　要：Solar corona is the outermost part of the solar atmosphere. Coronal activities influence space environment between the Sun and the Earth, space weather and the Earth itself. The total solar eclipse (TSE) is the best opportunity to observe the solar corona on ground. During the TSE 2008, a series of images of the corona and partial eclipse of solar disk were obtained using telescope and CCD camera. After image processing, preliminary results of coronal structure are given, and radial brightness profiles of the corona in directions of pole and equator of the Sun are measured. Though in solar activity minimum, the shape and structure of the corona are not symmetry. The equatorial regions are more extent than the polar one, and there are also larger differences between the east and west equatorial regions and between the south and north polar regions. Coronal streamers on east side of the equator, particularly the largest one in east-south direction, are very obvious. The coronal plume in south polar region consists of more polar rays than that in north polar region. These structures are also shown in other observations and data of SOHO. The radial brightness profiles in directions of pole and equator are similar to those of the Van de Hulst model in solar minimum, but there are a few differences due to coronal activity, which is shown in the isophote map of the corona.Solar corona is the outermost part of the solar atmosphere. Coronal activities influence space environment between the Sun and the Earth, space weather and the Earth itself. The total solar eclipse （TSE） is the best opportunity to observe the solar corona on ground. During the TSE 2008, a series of images of the corona and partial eclipse of solar disk were obtained using telescope and CCD camera. After image processing, preliminary results of coronal structure are given, and radial brightness profiles of the corona in directions of pole and equator of the Sun are measured. Though in solar activity minimum, the shape and structure of the corona are not symmetry. The equatorial regions are more extent than the polar one, and there are also larger differences between the east and west equatorial regions and between the south and north polar regions. Coronal streamers on east side of the equator, particularly the largest one in east-south direction, are very obvious. The coronal plume in south polar region consists of more polar rays than that in north polar region. These structures are also shown in other observations and data of SOHO. The radial brightness profiles in directions of pole and equator are similar to those of the Van de Hulst model in solar minimum, but there are a few differences due to coronal activity, which is shown in the isophote map of the corona.

关 键 词：太阳日冕 配置文件 日全食 结构 赤道地区 太阳能利用 北极地区 太阳大气 

分 类 号：P125.11[天文地球—天体测量] O532.1[天文地球—天文学]