Chase.] 112 [July 20, 1877. 
The following table gives a comparative view of the spectral and plane- 
tary series: 
Spectral Differences. Planetary a 
a 1.0000 14, 1.0000 4 g 
@ 1.0150 6 3 (a +7) 1.05384 45, 
Ocean a Figah8y Adon Ae a 
) 1.1986 a 4 (0 + ©) 1.2445 Is 
e 1.2904 a +(e + ¢) 1.3363 : 
¢ 1.3822 E 1 (€ + 7) 1.4281 2 
7 1.4740 a + (y+ @) 1.5199 Bp 
@ 1.5658 6 (O40) +2 1.6847 ‘ 
1 1.6576 i ha 
x 1.7494 x 1.7494 5 
A 1.8412 i abs 
p. 1.9330 a ba) =a 8 i 
y 2.0248 - (ev) 19789 
o 2.1166 Oto) +2 92.00386 8 | 
an = 2.2084 
In the fundamental harmonic denominators, it will be seen that @ = 
6 nm, and 6 is the figurate exponent of Jupiter in the equation of planetary 
masses. The value of 7 is the quotient of (Jupiter x perihelion radius- 
vector) by (Sun x solar radius). The significance of this quotient is ob- 
vious, on account of the preponderating influence of the two controlling 
members of our system. It becomes still more interesting upon examin- 
ing the portion of the spectrum which represents Jupiter’s most powerful 
reaction against solar action. 
As the harmonic basis is Jupiter’s present perihelion, it seems likely that 
there may be some changes in the relative positions of the spectral lines, 
with Jupiter’s changing eccentricity. As this change is less than ,+, of 
one per cent. per annum, its influence cannot be detected by direct obser- 
vation. But it may be worth while to institute careful comparisons be- 
tween solar spectra taken at our perihelion, aphelion, perijove and apojove, 
in order to find whether the lines are modified in any way by Earth’s posi- 
tion relatively to Sun and Jupiter. 
