EXACT ASTRONOMY. 



A Dynamical Resolution of the Solar Parallax. 



The conception of the solar horizontal parallax postu- 

 lates a circular orbit described with the radius R, equal to the 

 mean distance between the centers of terrestrial and lunar 

 revolution, measured by an arc x of the said great circle ; 

 equal in length to the earth's equatorial radius. If x be 

 taken in seconds, so must R be, and since the ratio of the 

 sidereal year in seconds T and R is constant, and that T = 

 /V * T , x R, it follows that factoring R factors T also. 



3X6 3 Xio 3 & 



Wherefore, the numerical expression of the mean radius of 

 the real elliptical orbit, by the ratio * compels the expres- 

 sion of the time of its description by the ratio J. Now, con- 

 ceiving resistance to the revolution of a planetary mass with- 

 out volume, at the distance i or x, eliminated by compres- 

 sion of the sun's volume, it would revolve in x seconds. 

 The proportion x 2 : x 3 : : T 2 : R 3 is consequently explicit in 

 Kepler's third law. 



Whence: x = -^ 3 = 8".8i 15507443 1 13. 



Also: II -7- ^ 8 = ~ = 1. 



x' x 3 R 3 



Multiplying the equation by ~, ■£ = !? = (-1-) 2 =(152.- 

 99822531 1 3 687) 2 = 23408.4569484283500. 



A Dynamical Resolution of the Equatorial Radius. 



The universal law of gravitation prescribes the multipli- 

 cation of the moon's sidereal period, t, by the square root of 

 1 -fm, the sum of the relative masses of earth and moon, the 



