Microwave observations of stratospheric ozone variations during a solar eclipse

During solar eclipses the ozone layer of the Earth is exposed to variable action of an ozone active radiation of the Sun (wavelengths 200-400 nm). The variations of magnitude and spectral structure of a solar ultraviolet radiation flow can cause both variability of total ozone content (TOC), and its vertical distribution. It is obvious, that the ozone variability should happen in the upper part of a layer (above than 40 km), where time of O/sub 3/ relaxation it is a little (photochemical time of life - about one minute). The ozone layer at altitudes of 40-80 km reacts most rapidly to variations of the Sun radiation, which are stimulated by rotation of the Earth (sunrise and sunset) and by solar eclipses. During eclipses the observations of TOC variations are carry out usually. The data of such observations represent rather inconsistent information about behavior of TOC to a phase of solar eclipses. It, most likely, is connected to that the full amount of ozone on heights exceeding 40 km, makes up only small part TOC. As to modifications of vertical distribution ozone density during eclipses, the information about them is not enough. The realization of similar observations has become possible due to emerging and development, perhaps, most approaching tool for research of the response of the upper atmosphere ozone on a rather rapid modification of the solar radiation - microwave radiometry with a high temporal and spectral resolution. We briefly present a method of research of ozone variations during a partial solar eclipse of May 31, 2003 (maximum phase about 70%), and discuss the used equipment and obtained outcomes.