When an approximate orbit is known in advance, we may use it to improve our fundamental equation. The following appears to be the most simple method:
Find the excentric anomalies and the heliocentric distances which belong in the approximate orbit to the times of observation corrected for aberration.
Calculate as in § I, using these corrected times.
Determine by the equation
in connection with the relation
Determine so as to make
equal to either member of the last equation.
It is not necessary that the times for which are calculated should precisely agree with the times of observation corrected for aberration. Let the former be represented by and the latter by and let
We may find as above, using and then use to correct their values, as in § VIII.
Numerical Example.
To illustrate the numerical computations we have chosen the following example, both on account of the large heliocentric motion, and because Gauss and Oppolzer have treated the same data by their different methods.
The data are taken from the Theoria Motus, § 169, viz.,
Times, 1805, September
5.51336
139.42711
265.39813
Longitudes of Ceres
95° 32' 18''.56
99° 49' 5''.87
118° 5' 28''.85
Latitudes of Ceres
-0° 59' 34''.06
+7° 16' 36''.80
+7° 38' 49''.39
Longitudes of the Earth
342° 54' 56''.00
117° 12' 43''.25
241° 58' 50''.71
Logs of the Sun's distance
0.0031514
9.9929861
0.0056974
The positions of Ceres have been freed from the effects of parallax and aberration.