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CARNEGIE INSTITUTION OF WASHINGTON. 



3. The following variables of long period belonging to the Algol and 

 Cepheid classes have been found to have bright lines. In most cases 

 the strength and appearance of bright lines vary with the light varia- 

 tion. The spectra of all of these stars show Cepheid characteristics 

 strongly, and there seems to be no means of determining the type of 

 variation from their spectra. Only one component is visible, but all 

 except RT Serpentis and RZ Ophiuchi show a considerable range in 

 velocity : 



4. The spectrum of Nova Aquilse 1918 and its surrounding ring has 

 changed but slightly in the last year. The ring has decreased in bright- 

 ness relatively to the central star, but the same twisted features re- 

 main in the nebular bands, Ni and N2. The bright extremities or 

 "knobs" of these bands and the band at X4686 are the only breaks in 

 the strong continuous spectrum of the nucleus. 



5. The spectrum of Nova Cygni 1920 was observed from August 22 

 to September 4, 1920. The early plates showed a spectrum similar to 

 that of a Cygni. Bright bands were prominent on August 25. Two 

 absorption components of the hj^drogen lines were measured on Sep- 

 tember 4. The displacement of the absorption lines other than hydro- 

 gen increased from — 6 a on August 22 to — 14 a on August 27. The 

 velocity of the star as determined from the sharp H and K lines 

 is —18 km. 



6. The spectrum of T Coronse, the Nova of 1866, is found to be of 

 type M with a very strong bright H/3 and a less pronounced bright Hy. 

 A bright line at X4686 is a marked feature of the spectrum. The 

 absorption lines agree closely in character and intensity with those of a 

 typical giant star of tj^'pe Ma. 



7. A few slitless spectrograms of Novse have been obtained by Mr. 

 Pease at the primary and Cassegrain foci of the 60-inch and 100-inch 

 reflectors. Those of Nova Aquilse 1918 show images of the ring in 

 light from the Ha and Ni and N2 lines. 



8. Fiirujhelm's distant companion to Capella was found to be an 

 Ma dwarf star with the same parallax and radial velocity as Capella 

 itself. The close companion of Antares is of spectral type B3 with wide 

 hazy lines. An excellent photograph of the spectrum of the faint com- 



