166 Proceedings of the Royal Irish Academy. 



tlie satellite, which is self-luminous ; or the observing body may be 

 supposed to consist of a cloud of meteors, so scattered that about 

 0' 1 1 of the light of the star can pass through them. 



The star has been examined with the spectroscope at Lord Craw- 

 ford's Observatory, and it was found that at the minimum the blue 

 end of the spectrum faded, and the red end was intensified. 



Knott has observed a small bluish star near the variable, and esti- 

 mated its position 60°, and distance 10". 



8. S Cassiopeia. — Schonfeld finds the increase of light consi- 

 derably quicker than the decrease. A star 9-6 m. follows 20^ and 

 2'S. 



9. S PisciuM. — Reddish. Elements derived by Schonfeld from 

 6 good maxima. He notes an 11 -12 n. star nf, and a 12 m. nearly 

 south of the variable. At minimum, Schonfeld says the star com- 

 pletely disappears in his telescope. 



10. E, ScxjLPTOEis. — Discovered to be variable at Cordoba. Dr. 

 Gould describes it as "one of the most brilliantly- coloured stars in 

 the heavens," its colour being "an intense scarlet." The observa- 

 tions show a variation from 5*8 to 7; 7 or lower, with a period of 

 about 207 days, and a symmetrical light curve. Maxima occurred in 

 December, 1872, and January, 1874 (two periods) ; and a Minimum, 

 1878, November 15 (mag. 7|-). It is No. 24 of Birmingham's Cata- 

 logue. 



11. E, PisciiJM. — Increase of light, according to Schonfeld, quicker 

 than the decrease, in the proportion of 4 : 5, but with fluctuations. 

 His observations between 1865 and 1869 give a period of only 337"5 

 days. He mentions an 11 m. star, nf, the variable. 



12 S Aeietis. — Schonfeld finds that all the observations indicate 

 a period of 292 days, but that this does not agree with observations 

 at Markree Castle, 1848, December 14; and by Winnecke, September 

 and October, 1868. The last observations, if correct, would show that 

 no regular period exists. 



13. E- Akietis. — Schonfeld says it has been well observed through 

 thirty-one periods, and often at minimum. The elements also repre- 

 sent the observations of Bessel, 1828, November 26, 8 m., and 1832, 

 December 15, 8-9 m. ; and also the supposed invisibility of the star to 

 Lalande, 1793, August 24. In some of the maxima, the light varia- 

 tion is very slow for some weeks. 



14. o (Miea) Ceti. — This is perhaps the most remarkable variable 

 in either hemisphere. It varies from a bright 2 m. to about 9 m. in 



