NEW STAR IN THE CONSTELLATION AURIGA. 



55 



Table — continued. 





Number 









Number 







1892. 



of 

 Observations. 



A. 



I 



1892. 



of 

 Observations. 



A. 



I 



Feb. 3, 4. 



2 



508-2 



2 F< 



sb. 5, 11. 



3 



468-0 



2 



„ 3, 4, 5, 11. 



6 



502-68 + 0-11* 



5 , 



, 5, 10. 



3 



466-8 



1 



„ 4. 



1 



501 + 



2 , 



, 4, 5, 10, 11. 



6 



465-4 



3 



,. 4, 11. 



2 



497-9 



1 



, 5, 10, 11. 



5 



464-3 



3 



„ 3,4. 



2 



494-7 



1 



, 4, 10. 



4 



463-3 



2 



„ 3,4,5,10,11. 



6 



493-17 + 0-17* 



5 



, 5, 11. 



3 



462-3 



3 



„ 3. 



1 



490 + 



1 



, 4, 5, 10, 11. 



5 



460-2 



3 



„ 3,4,5,10,11. 



9 



486-88 + 0-08* 



6 



, 4, 5, 10. 



6 



459-1 



2 



„ 10. 



1 



483-6 



1 



, 4, 5, 10. 



9 



457-8 



3 



„ 3, 4, 5, 10, 11. 



6 



482-0 



2 



, 4,5. 



3 



455-4 



2 



„ 4,5. 



2 



480-7 



2 , 



, 4,5. 



4 



453-8 



2 



„ 3,4,10. 



3 



478-8 



2 



, 4,5. 



3 



451-4 



2 



„ 4, 5, 10, 11. 



6 



477-41 



3 



, 5. 



1 



449-2 



1 



„ 4,5,10. 



4 



475-7 



4 , 



, 5. 



2 



448-0 



2 



„ io. 



2 



474-8 



2 



, 4,5. 



3 



445-5d 



3 



„ 3,4,5,10,11. 



7 



473-7 



4 , 



, 4,5. 



5 



442-1 



4 



„ 10, 11. 



5 



471-7 



3 



, 5. 



3 



439-4 



3 



„ 5, 11. 



2 



470-2 



1 



, 5. 



4 



435-5 



4 



„ 4, 10. 



3 



469-0 



2 











The lines marked d are double. All the measured lines are shown in fig. 1, where 

 the fainter grades are indicated by shortening the lines. In fig. 2 an attempt has been 

 made to represent the relative intensity of the various parts of the spectrum. 



In the spectrum the Sodium line (D), and the two Hydrogen lines C and F, are 

 present; Hy is very probably 435*5, which was just at the limit of visibility. All 

 these lines show a decided shift towards the red, from which I find the following velocity 

 of the body per second relatively to the solar system : — 



C,+ 211 miles, D,+135(±47) miles, F, 290(±31) miles. 

 The very bright line 517*45 lies within the magnesium lines b 1} b 2 , & 4 , and, considering the 

 shift of the lines, lies close to the iron lines b 3 , & 4 . However, the great intensity of the 

 line compared with that of the other lines of the spectrum, if iron be supposed to be 

 present, also the gradual falling away of the light towards the red, are in favour of 

 magnesium. The remaining two bright lines are not the nebulous lines. 



As the great intensity of the spectrum in the green, due to numerous lines, many of 

 which I was not able to measure, suggests the presence of iron in the Nova, I have entered 

 in the second line of the diagram the most prominent lines of the iron arc-spectrum for the 

 sake of comparison. Although a number of the lines fall together with those of the Nova, 

 one cannot lay much stress upon these coincidences, owing to the great number of lines 

 in Iron and the Nova scattered over the whole visible spectrum. 



* It was noted on Feb. 3 that the three lines, 502-7, 493*2, and 486-9, "look as if they are double." On Feb. 4, 

 the line 493-2 is entered as the " middle of two lines." 



" Dark spaces between the very bright lines" were seen on every night of observation from Feb. 3 to Feb. 11. 

 t More close lines in this place. 



