BF a 
1872.) 52) 
[Chage. 
AY 
nearly equivalent to the co-efficient of the exterior intra-asteroidal ab 
scissa (? 4 ). 
The co-efficient of the inner limiting planetary abscissa (4 & 5 8) is 
The co-efficient of the outer planetary abscissa {¢ X $ W) is nearly the 
reciprocal of the co-efficient of the inner extra-asteroidal abscissa (3 2J). 
The middle abscissa of the planetary series corresponds very nearly with 
the inner limit of the asteroidal belt (Flora = 2.674854), as well as with 
¢ of the mean distance of the three principal central asteroids 2.672519), 
5 I ( ? 
and with 4 of the geometrical mean between Flora and Cybele 2.683640). 
5 g y 
Between modulus and the influent centre of solar explosive oscillation 
(4 L) there are fifteen abscissas, of which § kh is the middle one, 
Between the Saturnian abscissa and jr, there are fifteen abscissas. of 
which 4 L is the middle one. : 
The abscissas representing centres of effluent or influent explosive 
condensation (§ M and } L), are similarly situated with reference to the 
intermediate planetary belt, 
No probable values can be assigned to the cardinal abscissas (4 Centauri 
and § L), which will produce deviations ef the theoretical from the ob- 
served values of a higher order of magnitude than the planetary eccen- 
tricities. 
Henderson’s first estimate of the parallax of g Centauri was 1//.16. 
Maclear’s observations, in 1839-40, gave /’,9128, and his more extended 
series, 1839-48, gave //.9187. Norton adopts ’,918 ; Lockyer, /’.9187; 
Denison, without assigning any reason, /’.976. We may reasonably re- 
gard Norton’s and Denison’s estimates as the limits of probable value, 
and compute the logarithmic 7 and ¢ from each estimate by the following 
equations. 
E+ 20% +400 £ = 7.686009 (N), or 7.657096 (D) 
&= 4L = 1.208919. 
b= yn + C—=-1.221849 
% ea et 
mee G 
d 
Solving these equations we obtain : 
= .211401 +, or .210702 + 
vf 
F = .005622 +, or .005585 4 
‘In the following table, C’ contains the abscissas accerding to Nor- 
ton; C’’, according to Denison; C’’’, according to the actual planetary 
mean distances. The degree of accordance, between the parabolas which 
are computed from stellar and solar data and the one which is computed 
from planetary data, and the evidences of «ethereal condensation which 
are furnished by the gradual lengthening of the observed abscissas, are 
especially noteworthy. 
A. P. 8.—VOL. XII.—3N 
