us*y: 
Partial Eclipfes , the Beginning and End , and in Total ones of 
ftiort continuance in the Shadow , the Beginning and End of To- 
tal X arkne& 5 ■■ are unfit for nice Gbfervadons, by reafon of the 
flow change of Apparences ? which the oblique Motion of the 
Shadow then caufeth. For thefe reafons I fliall propound a Me- 
thod peculiarly defign’d for the Accomplishment of the Geographi- 
cal end in Obferving Lunar Eclipfes , free (as far as is poffible) 
from all the mentioned Inconveniences. 
For, Fir(£> It fball not be pra&icablewithoht c Telefcope* 
Secondly , The Obferver fliall alwayes have opportunity before 
his principal Obfervation, to note the' 'Diftin&ion between the 
True Shadow and the Penumbra. And, Thirdly , It fliall be appli- 
cable to thofe Seafons of the Eclipfe , when there is the fuddeneft 
Alteration in the 
To fatisfie all which intents 7 
Let there be of .the Eminenteft Spots , difperfed over all Quar- 
ters of the Moons Surface^ a feled number generally agreed on, 
to be conftantly made ufeoff to this purpofe , in all parts of the 
World. As, for Example , thofe , . which M. Hevelius calleth 5 
Sinai,, 
tAEthna. 
Mom < 
P or phy rites, 
. ^Seromm, . 
Let in each Eclipfe., not all, but (for inftance) three of thefe 
Spots ^ which then lie neareft to the Echptick , be exactly obfer- 
ved , j when they are firft touch'd by the T rue Shadow , ancfagalp, 
when they are juft compleatly entred into it , and (if you pleafe) 
alfo in the Decreafe of the Eclipfe , when they are firft fully clear 
from the True Shadow: For the accurate determinations of which 
moments of time (that being in this bufinefsof main importance) 
let there be taken Altitudes of itmzxhihlsFixedStars •, on .this 
■ fide 
X Besbicm, 
Creta, 
'Palm 
Maotps, 
Mar a otis. 
Lacus Niger Major. 
