95 



Date 

 1894 Nov. 23 



30 

 Dec. 16. 



1895 J'ln 



3606 



96 



Ax 



3'.'00 2 



1.888 

 1.115 

 1.970 

 3.600 

 1 0.267 

 13 128 



- >"o35 



- 0.731 

 ■ 0.558 



- 1028 



- 2-057 



- 7-624 



- 'o 546 



Aft 



-o'.'oo9o 

 -0.0064 

 0.0049 

 •0.0086 

 - o 0165 

 -0.0531 

 -00706 



A(f 



-o'.'7 4i 

 -o 544 

 -0.415 

 -0.761 

 -1.484 

 -4.874 

 -6.415 



These quantities were then substituted into the differ- 

 ential formulae whose coefficients are given below and the 

 corresponding perturbations in a and d were found to be: 



Applying these perturbations with the reversed sign 

 to the normal place residuals, after the right ascensions of 

 the latter have been multiplied by the cosines of the decli- 

 nations we derive the residuals Undisturbed Position minus 

 Ephemeris. These are the absolute terms of the equations 

 of condition used in determining the definitive osculating 

 elements. 



Undisturbed Position — Ephemeris. 



23 

 30 

 16 



20 



27 

 19 



27 



I 

 II 

 III 



IV 



V 



VI 



VII 



Aa CO?, d Ad 



5 — 7:'28 —2:19 



5 -5-57 -HO. 32 



5 —0.20 -h3^:i 



5 -1-0.90 H-4.02 



5 -1-1.44 -1-2.86 



5 -<-4 03 H-9.88 



5 -(-6,90 -F4.20 



Date 

 1894 Nov. 23.5 



The residual in 6 for the normal place of Jan. 19.5 

 appears to be discordant when compared with those of th« 

 other normal places. That this is actually the case becomes 

 more certain when it is noted that all of the normal places 

 except this one depend upon from 5 to 13 observation.' 

 while this is based upon only 2, Nos. 68 and 69, and the 

 latter of these depends upon an assumed coincidence betweet 

 comet and comparison star. It was suspected that it wouli 

 be impossible to pass through the normals an orbit which 

 would give a good representation for the declination of this 

 date, and a preliminary solution proved this to be the case 

 Although the errors of the positions forming this norma 

 are not larger than those occurring in a number of othej 

 observations they are of the same sign, thus preventing com 

 pensation. A consideration of all the data led me to be 

 lieve that the retention of these observations as a separate, 

 normal place would add nothing to the accuracy of the 

 results. Nor did it seem advisable to combine them wit! 

 the normals of Dec. 27.5 or Jan. 27.5 on account of the 

 magnitude of the intervening intervals. The declinationi 

 were therefore excluded from the calculation while the righ 

 ascensions, not presenting any special discordance, were 

 retained and given a small weight. 



7. Differential Formulae and Least Square Solution 

 for Definitive Elements. 



Transforming the ephemeris positions of the come 

 for the dates of the normals to the ec|uinox of 1900.0, whici 

 has been choosen for the calculation, they become : 



Dec. 



1895 Jan. 



30 

 16 

 20 

 27 



19 

 27 



336° 35' 53 



341 43 40 



352 56 19 



355 37 46 



o 14 25 



'4 37 '4 



19 23 38 



■78 

 94 

 98 

 84 

 27 

 90 

 89 



These coordinates together with Chandler's elements 

 referred to the equinox of 1900.0 form the basis for the 

 calculation of the differential formulae, which, as has already 

 been stated, was carried oilt according to the method of 

 Schonfeld. The computation ()f these coefficients was checked 



by assigning arbitrary variations to the elements and deter 

 mining the resulting changes in a and 6 both by the differ 

 ential formulae and by tlie ordinary ephemeris formulae. 



0.5(42 



-+- 0.5 



0.6; 65 dJ/,1 -f- 2.3668,, dfi -+- 9.0488 dr/i 

 0.6148 -f- 2.2762,, -(-9.6080 



0.5:91 -I- 2.01 19,, -+- 9.9723 



74 



■-92571. 

 1-7397.. 



■+■ 0.0184 

 -+- 0.0788 



The equations of condition thus derived are : 



log V> 

 9.6572,, d.^ -t- 9.4308,1 dj' :^ 0.8619,1 0.3854 



9.6362,, -1- 9.48730 = 0.7459,, 0.5167 



9-5599.. -I- 9.56600 = 9-2967.. 0.4286 

 9-5354,. -*- 9-5773., = 99538 0.4722 

 94874.. -^- 9-5907.. == 0.1581 0.3702 



ii 



