Mr. Pigott’s Investigation of the Changes 
H 8 
5th View. 
The least brightness or minimum is represented by fig. 6, 
when the bright spots y and x at each extremity of the equa- 
torial diameter are mutually but just in sight and a minute one, 
r alone on its surface preceding y by 6 days motion : n n, are 
other middling sized spots near x, but preceding it; they 
cannot for the present be seen, being on the opposite or bright 
hemisphere. The spot x during the stars revolution having 
lost its light, and r being considerably increased, the next 
minimum will be between n n and r, (instead of x andy.) See 
fig. 7 ; and by the retiring of n n the diminution of the star’s 
light will continue to take place only until the reappearance 
of r, at the place where y was, which being 6 days sooner than 
the former position, (See fig. 6 , ) reduces the rotation to 56 
days. All the foregoing views are from unconnected periods, 
where only the ultimate returns of each appearance have been 
attended to ; but now, I shall examine a long interval with 
many intermediate changes, that between June 18th, and 
September 17th 1796, wherein are included the most intricate 
irregularities and vicissitudes : these observations are already 
printed at full length in the Philosophical Transactions for 
3 797, and therefore can at any time be inspected: indeed, I 
then little thought they would ever become of further use, but 
that of stating facts, to which, however, I have always been 
very partial, and particularly so, after having experienced the 
advantage of Maraldi’s printed observations on the variable 
star in Hydra, as it was partly by them that I ascertained the 
periodical returns of brightness of that star, and which flattered 
me the more, as Maraldi himself had been less successful in 
