8 ANNUAL RECORD OF SCIENCE AND INDUSTRY. 



eral catalogue so far as the double stars of W. Struve are 

 concerned. It is a careful collection of all the measures of 

 Struve in the "Mensurse Micrometrica?," and in the minor 

 works, and all these stars (above 3000 in number) are ar- 

 ranged in order of their right ascensions for 1875.0. For 

 each pair all the particulars of magnitude, color, distance, 

 position- angle, date of observation, even the magnifying 

 powers employed, are given, as well as the co-ordinates, 

 right ascension and declination for 1875. The precessions 

 are to be taken from a table appended to the book. The 

 full notes give further measures. Thus the particulars re- 

 garding each star are to be found collected on one line. If 

 a reference to Struve's own measures is desired, a column 

 gives the page of the original work where these may be 

 found. 



Flammarion, of Paris, has in the press a work on binary 

 stars, etc., in which all observations are given for each star, 

 and a discussion of their orbits, etc., follows. 



Burnham, of Chicago, has lately discovered some interest- 

 ing doubles, among which we may cite L 22020, pz=60, 

 8=0.5", mags. 9, 9; O. Arg. 11836, p = 80, s=l", mags. 

 8, 9 ; L 18231, p = 70, s=1.3", mags. 8.5, 10. These are re- 

 markably difficult stars to be found with a six-inch aperture. 

 Mr. Burnham also notes that 8 Sextantis=A. C. 5 is a rapid 

 binary, having moved 130 since 1860. 



It may be definitely stated that the new companions to 

 Polaris reported by Boe do not exist, as Mr. Burnham, of 

 Chicago, has examined this neighborhood with the 18-inch 

 refractor at Chicago without finding them. 



Struve and Dubiago, of Pulkova, publish in the St. Peters- 

 burg Academy Bulletin a new investigation of the orbit of 

 2 1728 = 42 Cornea Berenices. The orbit is based on thirty- 

 eight measured distances alone (the apparent orbit being 

 strictly a right line), and the observations are represented 

 with unusual exactness. The period is 25.71 0.080 years. 

 This orbit must be regarded as better established than that 

 of any binary. 



Gruber, of Buda-Pesth, gives the following elements for 

 "Eta Cassiopeice: Periastron passage, 1706.72; periodic time, 

 195.235 years; eccentricity, 0.6244; longitude of node, 33 20', 

 of periastron, 229 27'; inclination, 48 18' (1850.0). These 



