from an Eclipfe of the Sun • 
% 
P O S T S C RIP T. 
IN the month of February laft, I was favoured by Count 
be Bruhl with the obfervation of the eclipfe of the 4th of 
June laft, made at Warfaw by M. Bystrzyskx ; about the 
fame time I alfo received of M. de la Lande fome other obfer- 
vations of the fame eclipfe, viz. thofe made at Prague, Mar- 
feilles, Crefmunfter, and Bagdad in Mefcpotamia, which I 
immediately calculated, in order to add them to the others, 
which Dr. Maskelyne lately did me the honour of prefen t- 
ing to the Royal Society. 
The obfervation of Marfeilles confirms in the heft manner 
the difference of meridians fet down in the Requifte 5 Tables. P 
differing from that only by a fecond. The obfervation of 
Warfaw gives a difference ten feconds greater, and that of 
Crefmunfter fourteen feconds lefs ; which differences ought 
not to furprize us, confidering the obfervations upon which 
the longitudes of thefe two places had been eftabliftied ; hut, 
on the other hand, the obfervation of Prague dearly proves, 
that the fituation of that town had been much lefs accurately 
determined than one might have expedled. The time for the 
conjunftion, which refults from this obfervation, is the very 
fame as that which is deduced by M. Gerstner’s new method, 
defcribed in the Berlin Ephemeris for the year 1791, p. 243. 
From this time of conjunction the difference of meridians 
comes out equal to 57' 42^,7, viz. one minute and feveiiteen 
feconds lefs that that of the Requifite Tables. 
The calculation of the obfervation made at Bagdat feems to 
indicate that there is fome miftake with regard to the end of 
the eclipfe, having found, that the difference of apparent Ion- - 
si* 
