400 



Sir Norman Lockyer. 



Magnitudes of Nova Persei — continued. 







(1) 



(2) 



(3) 



(4) 



April 



5 



4 -8 (10. 0) 



4-5 



— 



— 



jj 



6 



5 -5 (8. 30) 

 6-0 (7.30) 









SJ 



7 . . . . 



5-5 



— 



z 



JJ 



8 



4 -2 (11. 0) 



— 



— 



— 





9 



4 7 (11. 30) 



4-5 



5-0 



4-8 F.E.B. 



J J 



10 ... . 



5-7 (8.45) 





5-5 





JJ 



11 ... . 



5 -8 



— 



5 '6 or 7 





" 



12 



F5-2 (8.45) 

 \4s -9 (9.40) 





5 3 



5-0 F F B 



" 3 



13 .. .. 



4-6 (11.30) 



— 



4 -3 (8. 0) 



— 



JJ 



14 ... . 



5 *4 (9.30) 

 f 6 -0 or 



— 



5-5 







:J 



15 . . . 



< fainter (8. 0) 

 [5 -S or 9 (10. 30) 



— 



6-0 



— 



JJ 



16 ... . 



5 -5 (11. 0) 



— 



— 



— 



JJ 



17 



5-2 (8.30) 



— 



5-1 (8. 30) 



— 



JJ 



18 



4-2 (9.0) 



4 -2 



4-2 



4-3 H.S. 



JJ 



19 . . . 



5-2 (8.0) 



— 



— 



— 



5) 



20 



5 -9 or 6 -0 (8. 30) 



<5-5 (8.25) 



5 -6 (8. 30) 



— 



JJ 



21 . . . 



6-1 (y.O) 



— 



6 -0 or 1 (9. 0) 



— 



J J 



22 . . . 



5-7 (9.0) 



— 



— 



— 



JJ 



24 



<5-5 (8.30) 



— 



— 



— 



JJ 



25 . . . 



5-7 or 8 (8.15) 



5 *7 



5-6 (9.0) 



— 



) J 



26 



5-6 (9.0) 



5 -5 (9. 0) 



5 -5 (9. 0) 





J> 



27 . . . 



4-4 (9.15) 





4 -5 (8. 0) 



4-4 H.S. 





30 .. . 



<5 -6 (9. 15) 



5 -8 (9. 40) 







May 



3 .. .. 



5- 7 (9.0) 



6- (2.15 a.m.) 









j> 



4 .... 



5-8 



5-8 





jj 



5 .. . 







5-6 





It is interesting to note that the length of the period of variability, 

 reckoning from maximum to maximum, began after March 27 to 

 increase from three days to four days. 



The two following maxima, after that of April 8, occurred on the 

 13th and 18th, so that the period became still more lengthened, namely, 

 to about five days. Further observations up to May 5 seem to 

 indicate that the five-clay period is shortening. 



Another interesting observed fact was that the light of the Nova 

 at the minimum on the 25th was more intense than at the preceding 

 minimum on the 21st, the estimated difference of magnitude at these 

 times being about 4-tenths of a magnitude. Unfortunately the 

 increasing twilight and the unfavourable position of the Nova make 

 it very difficult now to determine the magnitudes correctly. 



The two plates accompanying this paper illustrate graphically the 

 various fluctuations of the light of the Nova from February 22, when 

 it had not quite attained its maximum brilliancy, to May 5. 



The curve is drawn to satisfy as far as possible all the observations 

 made at Kensington. The dotted portions represent the possible light- 

 curve for those times when no estimates for magnitude could be 

 secured. 



In the plates the abscissae represent the time element and the 

 ordinates that of magnitude. 



