FIELD: physics.
SUBSTANCE: method involves determining the value of the relative radiation power of two stars. In the measurements, a charge-coupled device is used. The magnitude of the relative radiation power is determined by calculating the brightness in gray levels of the resulting image by summing the brightness of each of its individual pixels minus the background sky signal. At the same time, the angles between the horizon and the stars A and B are measured, along which the atmospheric mass is calculated for each of the two stars. The coefficient of atmospheric transparency is determined from the expression: 
where IA, IB - known anatomic temperatures of stars A and B; SA, SB - the relative powers of the radiation of stars calculated in the experiment; Ma, MB - atmospheric masses to the stars A and B.
EFFECT: simplification of the method, shortening the measurement time and providing the possibility of making measurements at any time of the day.
2 dwg
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