VARIABLE STARS. 175 



one gradat/on brighter than the star 17 Cygni. The fluctuations, how 

 ever, are in this case also very considerable, and have been observed 

 from thirteen gradations below the mean to ten above it. At this low- 

 est maximum the star would be perfectly invisible to the naked eye, 

 whereas, on the contrary, in the year 1847, it could be seen without 

 the aid of a telescope for fully ninety -seven days; its mean visibility 

 extends to fifty-two days, of which, on the mean, it is twenty days on 

 the increase, and thirty-two on the decrease. 



(4) 30 Hydra Hevelii, R. A. 200 23', Decl. 22 30'. Of this star, 

 which, from its position in the heavens, is only visible for a short time 

 during every year, all that can be said is, that both its period and its 

 maximum brightness are subject to very great irregularities. 



(5) Leouis R. =420 Mayeri ; R, A. 144 52', Decl. +12 7'. This 

 star is often confounded with 18 and 19 Leonis, which are close' to itj 

 and, in consequence, has been very little observed ; sufficiently, how- 

 ever, to show that the period is somewhat irregular. Its brightness at 

 the maximum seems also to fluctuate through some gradations. 



(6) v Aquihe, called also r) Antinoi ; R. A. 290 12', Decl. -j-0 37'. 

 The period of this star is tolerably uniform, 7d. 4h. 13m. 53s. ; observa- 

 tions, however, prove that at long intervals of time trifling fluctuations 

 occur in it, not amounting to more than 20 seconds. The variation of 

 light proceeds so regularly, that up to the present time no deviations 

 have been discovered which could not be accounted for by errors of ob- 

 servation. In its minimum, this star is one gradation fainter than i 

 Aquila;; at first it increases slowly, then more rapidly, and afterward 

 again more slowly ; and in 2d. 9h. from its minimum, attains to its great- 

 est brightness, in which it is nearly three gradations brighter than (3, 

 but two fainter than 6 Aquilm. From the maximum its brightness does 

 not diminish quite so regularly; for when the star has reached the bright- 

 ness of j3 (i. e., in Id. 10h. after the maximum), it changes more slowly 

 than either before or afterward. 



(7) /? Lyra;, R. A. 281 8', Decl. 4-33 11'; a star remarkable from 

 the fact of its having two maxima and two minima. When it has been 

 at its faintest light, one third of a gradation fainter than f Lyrae, it rises 

 in 3d. 5h. to its first maximum, in which it remains three fourths of a 

 gradation fainter than y Lyras. It then sinks in 3d. 3h. to its second 

 minimum, in which its light is about five gradations greater than that of 

 f. After 3d. 2h. more, it again reaches, in its second maximum, to the 

 brightness of the first ; and afterward, in 3d. 12h., declines once more 

 to its greatest faintness; so that in 12d. 21h. 46m. 40s. it runs through 

 all its variations of light. This duration of the period, however, only 

 applies to the years 1840 to 1844; previously it had been shorter in 

 the year 1784, by about2h ; in 1817 and 1818, by more than an hour ; 

 and at present, a shortening of it is again clearly perceptible. There 

 is, therefore, no doubt that in the case of this star the disturbance of its 

 period may be expressed by a formula of sines. 



(8) 6 Cephei, R. A. 335 54', Decl. -f-57 39'. Of all the known va- 

 riable stars, this exhibits in every respect the greatest regularity. The 

 period of 5d. 8h. 47m. 39is. is given by all the observations from 1784 

 to the preseut dav, allowing for errors of observation, which will ac- 

 count for all the slight differences exhibited in the course of the altern- 

 ations of light. This star is in its minimum three quarters of a gradation 

 brighter than t ; in its maximum it resembles i of the same constellation 

 (Oepheus). It takes Id. 15h. to pass from the former to the latter; but, 

 on the other hand, more than double that time, viz., 3d. 18h.. to change 



