( *34 ); 
for the Latitudes at the Sun. And the Inclination of the 
Orb of Mercury to the Plane of the Ecliptick (deter- 
mined by accurate Obfervations near his northern Li- 
mit) being 6° 59' 20", we compute the Diftance of the 
Planet from his Node, in the former o° 41' 7", and, in 
the latter, i° 4 '37"; which, being deduded from h s 
Heliocentrick Places refpedively, leave the Place of the 
afcending Node, in 1 677, 14 0 21' 3" , and, in 1723, 
» 15 0 o' 53" : So, that in 4 6 Years the Node isfound 
39' 70" forwarder in the Ecliptick ; which is but 1 1 30" 
more than the Praecelfion of the Equinox in the fame 
Time. We may therefore fafely alfume the Plane of 
the Orb of Mercury to be immoveable in the Sphere 
of fix’d Stars, and its afcending Node to be c s 15 0 41' 
from the firft Star of Aries. Nor can fo very llow a 
Motion (luppofing fuch to be) be fully defined, but by 
the utmoft Care and Diligence of future Aftronomers, 
after the Obfervation of many Ages. 
As to the reft of the Theory of this Planet’s Motion, 
I make his mean Diftance from the Sun , 38710 fuch 
Parts as the mean Diftance of the Sun and Earth is 
100000 and his greateft Equation 23 0 42' 37". The 
Efocha of his middle Motion, ineunte Anno 1723, 
flyl. vet. from the Equinodial Point, I make / 19 0 
J q> 3 1" ; and that of his Aphelion to the fame Time 
^ 13° 3' 34": the Aphelion movin ^fecundum Seriem 
Signorum , feven Minutes in eight Years. And thefe 
Numbers I prefume, may reprefent the Motion ot 
Mercury , with an Exadnefs equal to that of any of 
the other Planets ; perhaps as near as the Sun ' s Place 
by any Tables, or thofe of the fixed Stars by any Ca- 
talogue yet extant. < ' 
It were to be wilhed, that fome good Obfervation, 
like this, had been made of the like Tranfit of Mercu- 
ry at his other Node in April, where he was feen in- 
deed 
1 
