CALCVLVS ECLIPSIS SOLIS. ^SS 



Nunc ad corrediones inueniendas , producatur Tab. III. 

 3 A in 2; Yt fit A 2; = ^ , vnde diflantia O A ^'S- 8. 

 ^iminuitur particula ~ cof. O Az vndc calculus ita 

 fe habet 



Log.P 1:3.5418405 

 Lpg.cof.GAO=:9.977i^74 hinc ergo uafcitur corredio 



3.4990079 — o, 8^11. z 



Log.n=3. 5^39555 



L^ -9.9350524 

 ^^=0, 8611.S 



Deinde ex A ecliptka^ paraHela ducatur linco- 

 la A X znx , fiquidenfi in Longitudine nuUus error 

 commifTus eft , hinc ergo diftantia GA minuitur 

 particula x cof. A G A , corredio ergo hinc oritur 

 — o, 83(^2 8.X Denique ad eclipticam normaliter pona- 

 tur lineola Ay~j vnde diftantia 3 A augetur 

 particuia —j fin. A G A ideoque corredio hinc nata 

 eft =:o, 54B29.J. 



Tempore ergo Iiuius obferuationis diftantit 

 centrorum Solis et Lunae ob has corrediones dc- 

 buit elfe 



£Oo8^', $ — 0, 85is— o, Z^^x-^o, S^^j 

 quae ergo aequalis effe debet fummae lemidiame- 

 trorum 



1958,8^' ex quo obtinemus hanc aequationem fi- 

 xialem : 



5o''-:o, S^i.s-i-o, 83<J. x — Oi S^Sy 



Y y 2. ^uod 



