on the Planets Venus and Mars. 29 
The heliocentric latitudes obferved 1781 July 30, 1783 
September 26, 1785 July 29, 1786 July 1, 1788 May 6, 
are very near the greateft latitude ; the mean of the inclina- 
tions found on thefe days is 3 0 23' 40, "2, and very near the 
mean of all the obfervations f 23' 37", 7. The inclina- 
tion, or the greateft heliocentric latitude, may alio be found 
bv interpolation of the maximum amongft the obferved helio- 
centric latitudes. This maximum is found 1781=5° 23' 39" 
1783 = 
o° 2 2 
0 
' A \ " 
4 l 5 
i j86 
o' 
D 
2 3 ' 
the mean of thofe 
three maximums 3 0 23' 38", 6, which inclination may be 
depended upon to 1 or 2 feconds The inclination of the orbit 
of Venus has been fuppofed in the tables of M. Cassini, Dr. 
Halley, and M. de la Lande, = 3 0 23' 20", and the error 
of the tables + 1 8 ,6. 
III. The heliocentric longitude and motion of the nodes of Mars. 
In a Paper printed in the Memoirs of the Royal Academy 
of Sciences at Stockholm, I have determined the heliocentric 
longitude of Mars's afcendmg node— \ s. \f 54/ 2 4/', 2, m the 
year 1783, December 7, 20 h. 23' 39", mean time at Copen- 
hagen: the error of M. Cassini s tables — io / 35 » hb. 
Halley’s tables — 23 / 27 ^ of M. de i.a Landes tables 
- 4/ on". I refer the reader to that Paper (Kongliga Svenlka 
Vetenlkaps Academiens nya Handlingar, Tom. "V I. for the year 
1785, p.285 — 290.). The annual motion of Mars’s node 
may be found by comparing the following obfervations of the 
longitude of the node. In the column A the numbers are 
going upwards from the obfervation 17^3 ’ ■ the column I> 
the numbers are going downwards from the obfervation 1595- 
The 
