C 4SI ] 
time with exaftnefs. To this point of time affign in 
fome crude manner the moon’s parallax in longitude, 
by which a time may eafily be*afrumed, not very 
diftant from the vifible conjun( 5 lion. This may very 
.commodioufly be performed inftrumentally by the 
propofition, with which I ihall conclude this paper. 
' To this point of time compute the place of the fun 
and moon, alfo for an hour before and after, or rather 
for fuch an interval'of time as may include the whole 
^ipfer-and not too much exceed, of which an efti- 
mate.^may eafily be made by the forementioned pro- 
pofition here fubjoined. But all thefe places of the 
luminaries may- be deduced from the calculation for 
finding the true conjundtion, by means of the horary 
motions^' In’ the next place, to each of thefc points 
of time compute the diftance from the zenith and the 
place inithe ecliptic of the nonagefime degree. Then 
from each pofitioii of the nonagefime degree, compute 
by the method deferibed, the moon’s parallax in lon- 
gitude, her apparent latitude, and apparent diameter. 
” Fig. 7. After this, affuming upon anyftraight line, 
as AB, the point C for the fun, from thence lay down 
for the three points of the ecliptic, for vyhich the pre- 
ceding computations were made, the three diflances 
CD, CE, CF, which fhall be the meafures in feconds, 
taken from a fcale of equal parts fufficiently large, of 
the diftances of the moon from the fun in each, com- 
pounded with their refpedtive parallaxes in longitude, 
ib as to reprefent the refpedlive apparent diftances of 
the moon from the fun in longitude. Upon thefe points 
eredtthe perpendiculars DG, EH,,FI, for the moon's 
correfpondent apparent latitudes, and deferibe through 
thefe three points thearch of a circle, asreprefentingthc 
vifible way of the moon from the fun during the ecUpfe. 
M m m 2 Then 
