The post-explosion shock propagation in the central region of our galaxy (Q794848)

This paper presents a rigorous study of the influence of shock phenomena on the structure of the several disk compounds of our Galaxy. The shock has been assumed to be generated through explosion in the nucleus of the Galaxy. The existence of several gaseous rings and complexes which are experimently observed in the disk of our Galaxy can be easily explained as concentrated lyres of gas behind the propagating shock front. The shock propagating in the central region of our Galaxy heats up and condenses the gas there. The time taken by the heated gas to cool down to its original temperature and energy has been calculated. The results obtained are in full agreement with experimently observed data.