394 PROCEEDINGS OF THE AMERICAN ACADEMY 



about 50. Argelander's method of comparison is used. A copy of the 

 observations has been furnished to the Harvard College Observatory. 



Hg. These observations were made by Dr. K. Ilartvvig, formerly 

 of Strassburg, Germany, at present of Dorpat, Russia. Since his 

 removal to Dorpat, circumstances liave prevented Dr. Ilartwig from 

 making frequent observations of variable stars. 



Hn. These observations were made by the Rev. J. Ilagen, S. J., 

 at the Colk'ga of the Sacred Heart, Prairie du Chieu, AV^iscousin. The 

 instrument is a telescope by Merz ; its aperture is o inches. The 

 observations were made by the division mto tenths of the interval 

 between two comparison stars. A copy of the observations has been 

 furnished to the Harvard College Observatory. Messrs. Zwack and 

 Zaiser have taken part in the work as assistants. 



K. These observations were made by Mr. George Knott, at 

 Knowles Lodge, Cuckfiell, Hay ward's Heath, England. The telescope 

 employed was made by Alvan Clark and Sons; its aperture is 7^ inches, 

 and that of the finder 2 inches. The variable is compared with stars 

 differing little from it in brightness; the magnitudes of the comparison 

 stars, and sometimes the magnitude of the variable, are determined by 

 the method of limiting apertures. 



P. These observations were made by Mr. H. M. Parkhurst, at 

 Brooklyn, N. Y. The instrument is a telescope made by Fitz ; its 

 aperture is !) inches, and the magnifying powers emijloyed are <36 and 

 150. Many of the observations wi^re made by Argelander's method, 

 and the remainder with photometric apparatus devised by Mr. Park- 

 hurst, and partially described in the previous circular. A copy of the 

 observations has been furnished to the Harvard College Observatorv. 



Sk. Professor Safarik of Prague, Austria, has published a notice 

 of his observations of variable stars in the Vierteljrdu-sschrift dcr 

 Astronomischen Gesellschaft, XIX. 144, from which the memoranda 

 given in this circular are derived. 



Sr. These observations were made according to Argelander's 

 method by Mr. E. F. Sawyer, at Cambridgoport, Massachusetts, by 

 means of an o|)era-glass for the brighter stars and of a field-glass for the 

 others. The same plan of observation will be followed durmg 1885. 



W. These observations were made by Dr. F. Wilsing, at the Astro- 

 physikalisches Observatorium, Potsdam, Germany. The wedge pho- 

 tometer was en)ployed in part of the comparisons, but in such cases 

 estimates in grades of the difference in brightness between the stars 

 compared were almost always added. These estimates appear to be 

 somewhat more accurate than the photometric observations, whiHi will 



