433 



PHILOSOPHICAL TBANSACTIONS. 



[anno 1747-8. 



• Cassiopex. 



1727 September 9 



1728 17 



1729 June 8 



December 3 



1730 June 11 



December 9 



1732 January.. 8 



1733 .' . . 21 



1734 June 13 



December 1 1 



1738 23 



1740 June 2 



1747 February 27 



N. 

 S. 



N. 

 N. 



South of 

 34° 55' 



55"0 - 



30.8 



35.7 

 9.4 



13.8 



30.8 



49.2 



64.8 



(.2.8 

 105.4 

 176".3 

 169.1 

 332.3 



Preces- 

 sion. 

 9"0 



29.4 



43 8 



53.5 



64.0 



73.8 



95.4 

 116.0 

 143.8 

 153.7 

 234.0 

 262.8 

 397.0 



+ 

 + 



Aberra- 

 tion. 

 2"2 

 4.6 

 16.3 

 16.5 

 16.2 

 16.3 

 12.9 

 10.0 

 16.1 

 16,2 

 15.2 

 16.5 

 0.2 



Nutation. 



2"4 

 5.2 

 6.8 

 7.7 

 8.4 

 8.8 

 8.9 

 7.9 

 5.0 

 3.7 

 7.2 

 8.9 

 4.7 



+ 



Mean Dist. 

 South. 

 68"6' 

 70.0 

 70.0 

 68.3 

 70.0 

 68.1 

 68.0 

 69.1 

 69-9 

 68.2 

 65.7 

 68.3 

 69.6 



Though I have taken no observation of t Persei since the 22d day of January 

 174O; yet as this star is very near the zenith, and a sufficient number were 

 made about the times when the equation, resulting from the hypothesis, was 

 at its maximum; I judged it proper to insert some of them in the next table; 

 the last column of which shows how much the star's mean distance was south of 

 38° 20' on the 27 th day of March, 1727. Among near 60 observations I meet 

 with 2 only that differ from the mean of these, so much as 2"; and those differ 

 almost as much from the mean of others, that were taken near the same time: 

 so that the hypothesis seems to correspond, in general, with the observations of 

 this star, as well as with either of the foregoing. 



T Persei. 



1727 September I6 

 December 29 



1728 21 



1729 2 



1731 January 3 



J732 8 



1733 21 



1738 December 23 

 1740 January. . 22 



South of Preces- 



38° 20' 



60"1 



39.7 



22.5 



S. 0.2 



N. 8.2 



22.0 



34.6 



117.0 



1325 



sion. 



+ 7"4 



XI.9 



27.2 



42.0 



59.0 



74.8 



91.0 



183.4 



200.2 



Aberra- 

 tion, 

 - 3"2 

 (- 12.9 

 12.8 

 11.5 

 12.8 

 12.7 

 11.7 

 12.8 

 11.7 



+ 



After the last recited observations, it may perhaps seem needless to add those 

 of « Persei, which is farther from the zenith; but however, as this star lies very 

 nearly at an equal distance from the equinoctial and solstitial colures, and the 

 series of observations of it is somewhat more complete than that of t Persei ; I 

 shall insert one at least, for each year in which it has been observed; by which 

 it may appear that the hypothesis solves the phenomena of stars in this situation, 

 as exactly as in others: for if a mean be taken of the numbers in the last column 

 of the following table, which expresses the mean distance of the star south of 



