1888.] of the various Species of Heavenly Bodies. 



37 



being cut out by the continuous spectrum, although 564 asserts 

 itself by a brightening of the spectrum at that wave-length in Yogel's 

 sketch, and by a rise in his light curve. 



The line at 540 is the only line of manganese visible at the tem- 

 perature of the bunsen burner, while the 581 measurement of Vogel 

 is in all probability the 579 line, the strongest line of iron visible at 

 low temperatures. 



In this star, therefore, we have continuous spectrum from the 

 meteorites, and carbon bands, one of them appearing beyond the con- 

 tinuous spectrum in the blue as a bright band; bright lines of 

 hydrogen, manganese, and iron being superposed on both. There is 

 no absorption of any kind, the apparent dark band being due to 

 defect of radiation, as in Argelander-Oeltzen 17681. 



Vogel's results are given in the 1 Publicationen des Astrophysik- 

 alischen Observatoriums zu Potsdam,' vol. 4, No. 14, p. 17. 



Pickering's are published in the ' Astronomische Naehrichten,' 

 "No. 2376 ; ' Science,' No. 41 ; and quoted in ' Copernicus,' vol. 1, 

 p. 140. 



1st Gygnus. — B.D. + 35°, J$o. 4001.— The spectrum of this star 

 was observed by Messrs. Wolf and Rayet in 1867, but no measure- 

 ments of the positions of the bright lines were then published. In 

 the same paper, however, they give the measurements of the positions 

 of the bright lines in 2nd Oygnus (B.D. + 35°, No. 4013) which 

 they observed about the same time, and since the bright lines were 

 similar in these stars, the wave-lengths 581, 573, 540, and 470, may 

 be taken as indicating the positions of the lines in 1st Cygnus. They 

 also observed dark spaces between 470 and 486, and on the blue side 

 of 573. 



Dr. Yogel, of Potsdam, examined the spectrum of this star, and 

 has published his results in three ways, as a list of bright lines 

 given in wave-lengths ; as a sketch of the spectrum as it appeared to 

 him, and as a curve showing the intensity of the light throughout 

 the spectrum. 



His wave-lengths are 583, 571, 541, 486 (hydrogen F) for lines, 

 and a bright band from 470 to 465, with its maximum at 468. 



The sketch confirms these lines, while the light curve adds three 

 others to them at wave-lengths 507, 527, and 558. He also gives an 

 absorption-band between the 486 line and 470 band, and in his 

 sketch gives a darkening on the blue side of 570, this being also 

 indicated in the light curve. These dark spaces agree with the dark 

 spaces observed by Messrs. Wolf and Rayet. 



The bright band, with its maximum at 468, is the bright carbon 

 fluting commencing at 474, and extending towards the blue with its 

 maximum at 468, as photographed at Kensington, and the dark space 



