134 ASTRONOMICAL anp 
‘was ‘made upon the difc of the fun ; and towards the end of 
the eclipfe, it was obferved how much time paffed from the in- 
ftant when the diftance of the horns was fenfibly the fame, to 
the end of the eclipfe. It is in this manner that it was deter- 
mined, that about 1’ 20” mutt have intervened, between the 
true inftant of the beginning of the eclipfe, and the time when 
the impreffion was firft obferved. 
-At firft it was thought ufelefs to endeavour to obferve the 
quantity of the eclipfe with the quadrafit, becaufe of the flow- 
nefs. of. the. motien of the two planets vertically ; ; however, 
upon ‘reflection, it was thought that the tranfits of the horns, 
and of the limbs of the fun and moon acrofs the vertical wire 
only, would be fufficient to give the differences of the altitudes 
and azimuths of the centers of the two planets, and, confe- 
quently, their differences of latitude and ‘longitude. “Thefe 
were, therefore, obferved towards the end of the eclipfe, and 
at the fame time, the tranfits acrofs the horizontal wire were 
obferved, ‘but without hoping that they could be of any great 
~ advantage, for calculating the diftance of the centers. 
"In the firft obfervation, the tranfit of the apparent lower 
Horn acrofs the horizontal wire is a little doubtful: It may 
therefore be proper to perfer, in the calcule from this obferva» 
‘tion, the tranfit of the limb of the moon, and of the apparent 
“upper horn, acrofs the fame vertical wire. 
. In the fecond obfervation, the inftant of the tranfit of the 
“limb of the moon acrofs the vertical wire was omitted, through 
“hurry :— "Fo calculate it, therefore, we may make ufe of the 
š tranfit of the horn acrofs the fame wire. — 
CThelatt obfervation, being more complete, we may calcu- 
wei it by the one or Eus other method, indifferently ; or we 
| may 
