20

The INTRODUCTION:

the Sun, and in the same Quarter of theHeavens that he is in, never receding fromhim more than about I of a whole Circle ;and therefore she can never come in Opposi-tion to him; which would necessarily hap-pen,did she perform her Course round theEarth either in a longer or shorter Time thana Year. And this is the Reason why Venus isnever to be seen near Midnight, but alwayseither in the Morning or Evening, and atmost not above three or four Hours beforeKITSun-rising, or after Sun-setting. From thetithe*' cur Time of J’s superior Conjunction (or whenbe is above the Sun ) she is more Easterlystar. than the Sun, and therefore sets later, andis seen after Sun-fetting; and then she iscommonly called the Evening-Star. Butfrom the Time of her inferior Conjunction,till she comes again to the superior, she thenappears more westerly than the Sun, and isonly to be seen in the Morning before Sun-rising, and is then called the Morning-Star.

After the fame Manner we prove, thatMercury turns round the Sun, for he alwayskeeps in the Sun’s Neighbourhood, andnever recedes from him so far as Venus does;and therefore the Orbit of § must lie with-in that of J : And on the Account of hisNearness to the Sun, he can seldom be seenThe Orbit without a Telescope.

^kdes the Mars is observed to come in Opposition,Earm, and likewise to have all other Aspects with

the