[ 180 ] 



XXXIX. On tJie Solar Eclipse of May 1 5th, 1836. 

 Bj/ C. RUMKER, Esq, 



2\) the Editors of the Philosophical Magazine aiid Journal, 

 Gentlemen, 

 TN the calculation of this eclipse, the following method has 

 ^ been adopted : Suppose <^ to denote the geocentric latitude, 

 T the apparent time from noon, t the north polar distance of 

 the sun, tt the difference of horizontal parallaxes reduced for 

 the spheroidical figure of the earth, X parallax in longitude, /3 

 moon's apparent latitude — sun's latitude. 



3600'' 



H = 



([ 's relat. hor. mot. in M 



P f Noon in Green. 15 May 75° 53' 40''-6 R sun*s \ semidia- 



^ tor mean | Mj^j^jg^t 15 May 76 3 21 -0 ^ moon's J meter. 



S = K—r + g, D = R — r — §, where r is to betaken out of the 

 following table to be entered with h cotan <p cos t = tan m . , 



cos <p sin T = sm n , 



sin (5— 7») 

 tan 71 



= cotan r, 



sin n 

 sin r 



= cos h 



TT COS h cos (|u, + v) = A, TT cos h sin (ju^ + v) = parallax in lat. 



(v^(S^-f3^) + x)H = dr. 



The upper sign of v is to be used in the forenoon, the lower 

 in the afternoon. When the sun is in the descending signs 

 180°— jx is to be used in lieu of jtt. 



h° 134 



35|36 



o I o I o I o I o 



373839,40,41 



o o o ! o o 

 42 43,44 45'46 



0000 

 47|48 49,50 



0000 

 5l|52 53 54 



o ' o o I o I o 



55,56 57i58 59 



o o I o 

 606162 



— CO 

 00 icr> 



do ,6d 





O '<N 



6 !6 



C< 00 Ut F^ '00 



CO to lr^jO^|-^ 

 6 |6 6 6 '^ 



rM CO 



00 'CO 



Tf,<M t-'t-. ro 



uo :o "^ 00 (N 

 CI ht kp (p op 



o ''^ a> 

 lo'oo o 

 9^,9 i'?' 

 6j coico 



I measured at Hamburgh at the time of the greatest obscu- 

 ration, the distance between the sun's and moon's south limbs, 

 y 5T'*25, whence the apparent distance of centres is found 

 63"-9, and the apparent difference of latitude 64''-0, instead 

 of which the Nautical Almanac gives 70''*6. Hence it follows 

 that a correction of — 6''*6 must be applied to the latitude 



