t 



376 SCIENCE PROGRESS 



Eddington, A. S., Note on Sir Oliver Lodge's Suggestions, 

 Phil. Mag. 84, 163, 191 7. 



Lodge supposes that the extra electrical inertia due to 

 the motions of matter is not subject to gravitation. The 

 velocity of a planet relative to the sun is compounded with that 

 of the motion of the solar system as a whole through space, 

 which gives an inertia alternatively increasing and decreasing. 

 This leads to changes in the perihelion and eccentricities of the 

 orbits. The anomaly in the motion of the perihelion of Mercury 

 might thus be explained. Eddington shows that, if this is so, 

 other anomalies in the motion of the Earth and Mercury would 

 be introduced, so that the suggestion is untenable. 



Variable and Binary Stars. — Shapley, Martha B., Light 

 Curves and Orbital Elements of TT Lyrae and 7 Camelop., 

 Astroph. Journ. 46, 56, 191 7. 



Baker, R. H., The Eclipsing Binary Z Vulpec, Laws Obs. 

 Bull. No. 26, 1 91 6, The Eclipsing Binary <o Herculis, Laws Obs. 

 Bull. No. 28, 1917. 



Cummings, Edith H., The EclipsingBinary, . Cassiop., 



Laws Obs. Bull., No. 27, 191 7. 



Wilson, H. C, Light Curve of T Androm., H.A. 80, No. 8, 

 1917. 



Russell, H. N., Fowler, M., and Boston, M. C, Com- 

 parisons of Visual and Photographic Observations of Eclipsing 

 Variables, Astroph. Journ. 45, 306, 191 7. 



Osthoff, H., Bemerkungen zu Argelander's Methode der 

 Schatzen's der Sternhelligkeiten, Ast. Nach. 4897-98, 191 7. 

 A valuable discussion of the various sources of error, mainly of 

 a physiological nature, which are liable to occur in the use of 

 Argelander's step method of comparing the brightness of stars. 



Lau, H. E., Untersuchungen iiber die Farben der Fixsterne, 

 Ast. Nach. 4900-01, 1917. 



Stellar Distribution, etc. — Miller, J. A., Determination of 

 the Parallaxes of 50 Stars, Sproul Obs. Pubs., No. 4, 191 7. 

 This paper contains the first series of parallax results obtained 

 at the Sproul Observatory together with a description of the 

 instrument and of the methods employed. A 24-inch refractor 

 is employed and the method of determination follows generally 

 the photographic method as employed by Schlesinger. The 



