SOLAR ECLIPSE, MAY (J, 1883. 137 



The plan of observations laid out by Dr. Hastinc^s was a.s follows: 



(1.) To observe the reversal of the Fraiinhofer lines an«l ciuleavor to estimate their dnration 



(2.) To note what lines persisted longest after the reversal. 



(3.) To search for faint red lines below in the spectrnni of the chromosphere, and two faint 

 green lines between 1)3 and 1474 of the coronal spectrum. > 



(4.) To search for dark lines in the coronal s])e(^trum. 



I failed to detect at the beginning or the end of totality, the reversal of the Frannhofer 

 lines; at tlie beginning of totality they disappeared in.stantaneously, and the dazzling, continiions 

 spectrum of the sun was as suddenly greatly diminished in brightness ; at the same time tlie briglit 

 lines of the chromosphere made their appearance, lasting but a few secoud.s, when they disappeared 

 gradually and simultaneously, with the excei)tion of the line 1474. This increased steadily in 

 brilUaney, while the continuous spectrnni grew fainter. A few seconds after the disappearance of 

 the chromos])heric lines, a light cloud passed over the eclipsed sun, and after its passage I began 

 my search for the phenomena I wished to observe. There was only the blight line, 1474, visible, 

 and this was intensely brilliant. I was greatly perjilexed by the absence of all other bright lines, 

 and I searched for a long time in the red, yellow, and green, without taking note of the time, think- 

 ing the other coronal lines might be very faint. AVhile engaged in this I detected what appeared 

 at first to be faint dark lines in the orange red. This appearance of there being several lines, lam 

 now inclined to ascribe to the fact that the line was very faint, and appeared only at intervals, dis- 

 apxiearing and again reappeariug in quick succession. This I saw several times during the first 

 lialf of totality. As Mr. Fletcher called out 190, I began to fear that the spectroscoije slit might 

 be too narrow, and widened it; after this I did not see the dark line. 



As there continued to be visible only the one line, and as I had searched thoroughly for others, 

 I began to experiment with the slit width, but succeeded in bringing out nothing else. While en- 

 gaged in this I was greatly surprised by the reap])earance of the bright lines of the chromosphere. 

 In ray anxiety I had ceased keeping track of the time, and at first mistook them for the other bright 

 lines for which I was seeking. While comparing them one with another, in order to determine their 

 relative magnitude, I observed a very faint red line a little less refrangible than C. But just at 

 the time I picked up this line, I became aware of their true nature by hearing Mr. Fletcher call out 

 that the eclipse was over, so that I obtained only a momentary view of it. The lines visible at the 

 time were (7* (which 1 did not examine closely) ; F, a very bright blue ; 1474, a dazzling line in the 

 green, but not so bright as it had been during mid-totality; l)j, a bright, yellowish-green line; C, 

 a broad and very bright red line; just a little below U was the faint line of which I liave spoken, 

 and which, though very little brighter than the red of the continuous spectrum, was distinct from it. 



As I thought at the time these lines were those of the coronal spectrum, 1 estimated their relative 

 rightness in magnitude, as follows: 1474, 1; F, lio; C, 2; D3, 3; CI, 1 



They lasted between 20 and 25 seconds; Mr. Fletcher had but shortly ceased calling out the 

 time, and tjie end of totality took place 35 seconds after his last call. 

 II. Computation of contacts, and observed times of contacts. 

 Using the approximate position of Caroline Island (Lat. 10° 0' 1".30 South, Long. 150° 15' 00" 



West), I computed the times of contact as follows: 



I. lO'' 3" aS^"" L. M. T. 



II. 11 ;il 50.04. 



III. 11 37 21.24. 



IV. 1 10 33.'-. 



• Thi.s line Is not G, but the line of li. (lroj,en just below G.— E. S. H. 

 S. Mis. 110 IS 



