Astronomy.

j 1 * 111 in the Times and Distances follow-

er viz.

The

so

Of

other M,

stfrd

* 5 - S

C , oursc there can be no Clouds, Rain, Snow,

P e ctcd eteorSy w ^ ence Changes might be ex-

the ^j o ° Inc f ( as we have shewn) the mean Distance of

th

S

Sift

°°n is about 60 Semidiameters of the Earth, at

Ursa.

ance of the Moon one Degree of the Earth’sthere's 6 ' Vl ^ frhtend an Angle of one Minute, and will^ilcs^V 36 visible ; but such a Degree is equal to 69!te r i tl ’,j ,ert ' f °re a Spot or Place 70 Miles in Diame-16 w^fr° on will be just visible to the naked Eye,tinries" %l ence a Telescope that magnifies about 100of * just discover a Spot whose Diameter is r ’ 5les Co j| es 5 or ot a Mile, or 3698 Feet: And a Te-jy6t , at will magnify 1000 times will strew an Ob-is b ut at Is b ut r £ c of a Mile, that is, whose Diameterste re f 37 ° Feet, or little more than 120 Yards; andeVe t> a o Vv *^ easily strew a small Town or Village, orXy ,P en tleman’s Seat, if any such there be.stg ’ ^ he Time which the Moon takes up in mak-Staj- f r * e Revolution about the Earth, from a FixedRd H, 0 *h? fame aj

the n T Ile a g a,n > ' s 2 7 d - 7 h- 43 % which is cal-De tw ee ° er *°dical Month. But the Time that passestyoo n tw ° Conjunctions, that is, from one New• S c alled n0ther ’ equal to 29 d. 12 h, 44/ 3", which15 htiin ? Synodical Month: For after one Revolutionbet le<a ’ the Moon has a small Arch to describe toe Ps _% eeu the Sun and the Earth, because the Sun"Utpl u Van cing forwards in the Ecliptic. Now thisst th e pOs Motion takes up 2 d. 5 h. 1 3", which addedst the eri0( lical Month makes the Svnodical, according18. ^ an Motions.

Tim e fb 6 . 0011 moves about its own Axis in the fameCort ies ^ ^ moves about the Earth, from whence itst : f Q that stie always strews the fame Face to

PP her S f ^js Motion about her Axis just so muchl £ t Mot" 11 " 366 * S turned towards us constantly, ashyIon ab out the Earth r^ould be turned from us,

I 4 19, But

119