Rocket UV flash spectra from the solar eclipse of March 7, 1970

Flash spectra of the total solar eclipse throughout all its phases have been obtained in the extreme ultraviolet for the first time.     

X-ray photographs of the sun on March 7, 1970

The Sun was photographed from an Aerobee rocket by means of equipment responding to the wavelength interval 3-60 angstroms, revealing interesting relationships between structures in the corona.     

日月食限的计算

日月食的观测对太阳物理学、天文学及其它相关学科的研究有重要意义．然而准确的日月食预报却离不开日月食限的计算．本文研究了日月食计算方法，力求简单易懂，以便于课堂教学和进行科普教育．     

日月食观测在科学研究上的意义

阐述了日月食观测在研究太阳大气结构、太阳活动，寻找近日彗星和水内行星，检验广义相对论理论以及校正历史中年日次序诸多方面的价值．     

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

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.