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6 the morning ; that he attains his greatest elevation in the sky at twelve ; and that he sinks below the western horizon between four and eight in the evening. We observe the same also with respect to the Moon; but the times of her rising and setting vary much more, according to her situation with respect to the Earth. If we watch the Stars, we shall see some of them rising and setting in the same manner ; but those which are near the pole never set; and one star may be observed which nearly occupies the place of the pole, and scarcely changes its position at all. This is called the Pole Star. If we watch the stars still further, we shall see a few of them which change their places with regard to the others ; these are called Planets , whilst the others are denominated Fixed Stars. The earliest, and what at first sight appears the simplest, method of accounting for these appearances, was that afterwards defended by Ptolemy (who flourished about A. D. 100), and called after him the Ptolemaic system. DIAGRAM I. Ptolemy considered the Earth to be in the centre of the system, and that the wfhole starry sphere revolved around it in 24 hours ; but that the Sun, Moon, and Planets revolved around it in periods varying more or less from that time ; the Moon being the nearest, then Mercury, Yenus, the Sun, Mars, Jupiter, and Saturn. This system, notwithstanding many palpable errors, maintained its ground for 1500 years; until Coperni- cus, a Polish Astronomer, revived the system believed to have been taught by Pythagoras about B. C. 500, but which had been relinquished on account of its apparent difficulties. Copernicus taught that the Sun is fixed in the centre of the system, and that the Earth and other planets revolve around him at different distances, in different periods of time, and with different velocities; that the Moon revolving round the Earth