48 



PHILOSOPHICAL TRANSACTIONS. 



[anno 1744. 



A series of observations is then given, of the right ascensions of the comet, from 

 which were calculated the following table of the places and elements, with the 

 differences between the observed and computed places. 



By the help of these observations, which were made by the Rev. Mr. Professor 

 Bliss, the transits excepted taken at Sherbom, Mr. Betts, by the method delivered 

 in the 3d book of the Principia, determined the comet's parabolic trajectory ; and 

 found the place of the ascending node to be in y 15° 45' 20'; the logarithm of 

 the perihelion distance 9,346472; the logarithm of the diurnal motion 0,g40420; 

 the place of the perihelion :Ch 17° 12' 55"; the distance of the perihelion from the 

 node 151° 27' 35"; the logarithm sine and co-sine of the inclination of the orbit 

 to the ecliptic, 9,865138, 9,8326l6; and thence the time the comet was in the 

 vertex of the parabola, or the time of the perihelion, Feb. ig'' 8'' 12"; the mo- 

 tion of the comet, in its orbit thus situated, was direct, or according to the order 

 of the signs. 



From these elements, by the help of Dr. Halley's general table, to which they 

 are adapted, Mr. B. computed the comet's places for the times of observation, 

 exhibited in the following table : to which are added the comet's longitudes and 

 latitudes deduced from the observed right ascensions and declinations ; with the 

 errors between the observed and computed places ; the observations being all re- 

 duced to Oxford mean time. 



Diff. in 

 Latit. 



26"- 



18 — 



14 — 



10 



31 



24 



18 



20 



34 



37 



29 



35 



18 



35 — 



37 - 



31 — 



28 — 



24 — 



+ 

 + 

 +■ 



+ - 



+ 

 + 

 + 

 + 

 + 



Perhaps it may hot be thought improper to remark, that the nodes of the 

 comet, and the planet Mercury, are situated within less than half a degree of each 

 other; which probably gave rise to a report, that the comet had carried Mercury 

 from its orbit. In order therefore to find how nearly they approached each other, 



