SOLAR ECLIPSE, MAY fi, 1883. 135 



account of the overlai)i)iiig of tlie rings. The absolute widtli of any one of the rings was not 

 estimated at the time, but it was recalled shortly after the eclipse that the width of the green 

 ring was about equal to three quarters of the distance betAveeu E and F, as seen with the same 

 prism and telescope. 



At the expiration of two hundred seconds of totality, immediately after the above obscuration, 

 it was noted that the red ring was decidedly the brightest, and it continued to increase in bright- 

 ness relative to the others during the next sixty seconds. In this interval, also, three spots of 

 light were seen, red, yellow, and green, due to solar prominences, and when two hundred and ninety 

 seconds had passed, the four curved lines seen at the beginning of totality were again observed. 



The phenomena attending the reversal of the lines were especially noted at the close of the 

 totality, the reversal not being seen at the beginning of totality either on account of the removal 

 of the dark shade at about that time or on account of clouds which may have then prevailed as 

 they were seen a few seconds later. As the end of totality approached, a large number of narrow 

 bright lines were seen and observed for several seconds before the corresponding dark lines 

 appeared. The change was instantaneous, or nearly so, the bright lines having been seen for an 

 interval estimated as five seconds, the wind preventing the chronometer beats from being actually 

 counted. 



During the second partial phase the dark lines were seen for twelve minutes after the end of 

 totality. 



In making the above observations I was assisted by Ship's Printer T. J. Brooks, of the U. S. 

 S. Hartford, who acted as recorder. 1 dictated to him occasional woixls at intervals during the 

 totality and also the corresponding times as announced by Mr. Fletcher. From these records, 

 which were written out more fully during the second partial phase, the above report is derived. 



OBSERVATIONS OF THE FIRST AND FOURTH CONTACTS. 



These were made with the 2i inch glass used in the spectroscope observations, but with a mag- 

 nifying power of 63. The time was recorded by Mr. W. B. Fletcher with chronometer Hutton 

 202. The following is the record : 



FIRST CONTACT. 

 /(. m. S. 



— — 23. Suspected; uot verified. 



— — 33.5. Suspected ; not verified. 



— — 4L5. Suspected; not verified. 



1 48..'i. Seen; not too l.ate by more tliaii 2». 



The chronometer had a correction of + O^.S on local sidereal time. The above time reduces to 

 10" 3™ 38«.0 local mean time. 



FOURTH CONTACT. 



9. Still seen. 

 14. .Still seen. 

 KJ. Sharp piojectiou on the moon's disk goes off. 



The chronometer had a correction of -f 9».5 on local sidereal time. The above time reduces to 

 !'■ 10"" 35».0 local mean time. 



It will be observed that this observation is about ten seconds earlier than those of the other 

 observers of fourth contact. This discrepancy I can explain only on the supposition of an error 

 of 10» by the time-keeper. The observation was peculiarly good on account of the sharp projec- 

 tion noted on the moon's disk, and could scarcely have been in error 2* as the definition was good. 



