Gore — On Knoicn Variable Stars. 173 



21. A TATjfii. — A star of the Algol type, but not so well observed 

 as Algol, The greater part of the light change is accomplished in a 

 period of about 10 hours. The inequalities in the period are consider- 

 able, sometimes amounting to three hours. 



22. T Tatjui- — North following d' Arrest's variable nebula. Schon- 

 feld can find no regular period, and remarks, with reference to its 

 colour, " Mcht auffalend gefarbten." 



23. E Tatjei. — The period is, according to Schonfeld, subject to a 

 variation of fifteen days ; but still the elements correspond with the 

 supposed invisibility of the star to Bessel, February 13, 1822, and an 

 estimation by Bode (7 m.), February 6, 1798. The increase of light 

 from 10 m. occupies about 37 days, and the decrease 47 days. Schon- 

 feld says : " Im minimum nach Winnecke selbst fiir das 7^ zollige 

 Objectiv des Pulcowa-Heliometers unsichtbar." Hind and Gold- 

 schmidt call the star red; "Winnecke, ''triib roth" ; Secchi, "orange- 

 gelb " ; and Schonfeld, " sehr roth." 



24. S Tatjei. — Period seems diminishing. Only for about 70 days 

 of its period is the star brighter than 12 m., which renders it difficult 

 to be observed. 



25. E DoEADtrs. — Discovered to be variable by Thome at Cordoba. 

 Dr. Gould says it is "excessively red." 



26. Y Taxjej. — Schonfeld calls it ''rothlich, " and says, "die 

 Yeranderungen sind rasch " ; and he thinks that a period of 171 'S 

 days nearly as admissible as that given in the Catalogue. A 12'13 m. 

 star follows the variable. 



27. E Eeidaisti. — Yariation independently found by three observers 

 at Cordoba ; but Gould gives no period, owing to insufficiency of ob- 

 servations. 



28. E Oeionis. — According to Schonfeld, the increase of light 

 from 10*2 m. occupies 70 days, and decrease 105 days, but both with 

 marked fluctuations. Hind calls its colour "reddish"; Schonfeld, 

 " stark rothlich " ; and Secchi, " gold^elb." 



29. 6 Atjeig^. — Schonfeld thinks there is no regular period, and 

 says that the variation is often for a long period imperceptible. 



Schmidt finds from his own observations, 1843 to 1875, that the 

 star is irregularly variable, and only within narrow limits. 



I observed e to be almost exactly equal to rj Aurigte on the follow- 

 ing dates: — 1875, December 21 : 1876, March 21 ; 1876, ISTovember 

 20. On 13th March, 1883, and 2nd April, 1883, I estimated its mag- 

 nitude as 3"57 (from comparisons with t] and ^ Aurigee). 



