Değişen Yıldızların Minimum (veya maksimum) Zamanı Gözlemleri

Abstract

The light changes in variable stars have certain physical causes behind. In order to understand the physical causes, the light changes have to be observed systematically and simultaneously in different filters. On the other hand, any change in the physical mechanism causing the lihgt changes can be detected by the observations of minimum or maximum times. Even the unfiltered observations are usefull fort his purpose. For example, the rotatinal changes or seular changes in the magnetic cycle of a magnetic star; the secular changes in the pulsation period of a pulsating variable; the mass distribution around a pulsating variable; information about other star or planets in its gravitational field; the secular orbital period changes of binary stars and the physical causes of these changes; the changes in the rotational motions of the Solar System members can all be detected by the analysis of minimum or maximum observations. Therefore, the minimum or maximum observatins of any celestial object are very valuable. But, in order to extract information from such observations, they have be to systematic, accurate enough and distributed evenly in a long time base. One of the must important contributions of amator astronomers in the advances of observational astronomy must be the minimum or maximum observations of different celestial objects.