Chase] 420 [Oct. 6, 



but subjected to invariable laws which are 'regulated bj'^ the relative 

 movements of the disturbing bodies. Xaumann's tables {Handbuch der 

 Chemie, 1877, pp. 346-59), show that if the whole Earth Avas a solid 

 diamond, or if it was composed of rocks which are least expansible, 

 the greatest quarter-daily tidal deformations would not involve an 

 amount of work equivalent to |o C. The spring tidal stress during six 



(m. ^a\ qP 

 -3 + — ^ I -^ =^ 619 ft., which is enough to furnish many 

 Ps pa / "^ 



times the available force requisite for all the adjustments of sethereal elas- 

 ticity, freely moving particles, and internal work in the solid rocks. 



268. " Conservation of Solar Energy." 



. The views of Dr. C. "William Siemens suggest a consideration of the in- 

 fluence of solar rotation upon the ajthereal atmosphere, at various dis- 

 tances from Sun's centre. Laplace's limit, according to the data in Note 

 263, is at 36.35 r^. The centrifugal force of rotation at that limit would be 

 36.35^:= 1321.3 times as great as at Sun's surface, while the centripetal 

 force of gavitation is only ig-^Vrs- times as great. The photographs of the 

 solar eclipse which have been lately published {Nature, April 20th, 1882), 

 indicate an atmospheric oblateness which may be due to the equilibrating 

 tendencies of these two opposing forces. If the sethereal disturbances 

 which result from this source are not sufficient to account for luminous 

 and thermal vibrations, we may look still further to the velocity which 

 the subsiding particles would acquire in falling from the equatorial 

 limit to the poles. If there was no resistance, this velocity would be 



/35.35 \^ 



( gg-og X 2^?' I = 376.8 miles per second. Any diminution of this 



velocity by resistance would be converted into heat. If ^the mean limit 

 between the centrifugal and centripetal tendencies is in latitude 30^, 

 the mean diminution of velocity when the particles reach the polar zone, 

 would be .982 of 376.8 = 370 miles. If the mean time of accomplishing 

 the centrifugal and centripetal cycles is the same as the time of half- 

 rotary oscillation, the formula of torsional elasticity (Note 162) provides 

 for radiations Avith the oscillatory velocity of light, and the general ten- 

 dency of nebuhe to a discoid or flattened form gains a new significance. 



269. Another Test of Atomic Divisors. 



In order to avoid all questions of absolute probability, in Notes 171, 

 201, 202, etc., I have computed (?i D — O) -r- D for all the elements in 

 Clarke's table except H, using Dj = 7 for the perissads, Dj = 8 for the 

 artiads, ©3 = 1 for the Hydrogen divisor. Adding the logarithms of 

 (» D — O) -^ D, I find for the perissads, 



2' (for D,) = A To". 4692966 



I (for D3) = B 2^.9326580 , 



A — B 1.5366386 



