SEPT See TT ee ee ee ee gTO eee 
Yi; Se tae ee a ee Ne eee See Se ee 
Be al i a 
‘Observations of the comet of 1807. 13 
a(31)= 35-p—244 x(7) = 14*p4. 79 
x(13)= 39:p—258 —x(2%)= 88+ p4522 
x(i*)= 80p~—493 —x(?*)= 42+p4291 
a(*) = 22*~—105 ax(4°)= 29° p4+203 
2(33)= 42-p—148 x(49)= 68° p+489 (G) 
—2z(?) = 67-p—181 —x(25)= 2994313 
x(*) = 26p— 68 x(48)= 73° p+835 
_x(?°)= 49:p—103 . -w(4?)= 26° p4+325 . 
x(34)== 16:p— 32 . —x(48)= 7 p+i02 
—x(3*)= 39p— 75 (22) 22+p4327 
= a(?*)= 55p— 72 —x($4)= 17-p 4426 
(88) 24p— 25 a(4#)= 16-ppssd 
Ba 32 p— 30 a8 ime ~x( *)s 14*°p4909 aaa 
— ey = ‘58p— 50 
—2(2°)= 66p— St uy! Slee 
—z(*) = 51p— 36 
The sum of all the coefficients of f in these equations is 2211, which 
.put=F. The sum of the first thirty of the coefficients is 1062, which 
is less than 3 F, and by adding the next coefficient the sum becomes 
1137, which is greater than } F, hence by the rule given by La Place 3 
the value of p, which will render the sum of the errors x(?), (*), &e, 
taken Be pOSve 2 a minimum will be found by putting the second mem. 
ber of the thirty - inst f the « uation (G)e equal to ( 0; that i is, 75 ‘p— 
52 60, which gives ete By substituting this value i in the equa- 
tions marked (4), (3), (2), (1), we successively obtain. as 
_N=0°49828-p-+0°80842=1°-154, : 
" d=0°58044" p+0°91 378*n—0°86191=0° 595. 
i= —0°22944-d40°15555-p+0-06885-n+40°30130=0°352. 
t= —0-40480-d-40°47493 ‘P+0°24398-n40°55366:-—0°02703=0°537. 
These values being substituted in the preceding expressior te : 
ements of the orbit, they become | 
3 
