  The spectrum of Nova DQ Herculis (1934) in 1950.Swings, Polydore  ; in Astrophysical Journal (1952), 116 Seven spectrograms of Nova DQ Herculis obtained in May and October, 1950, reveal that the striking changes in the spectrum of the nebulosity observed between 1942 and 1949 continue, while the mean ... [more ▼] Seven spectrograms of Nova DQ Herculis obtained in May and October, 1950, reveal that the striking changes in the spectrum of the nebulosity observed between 1942 and 1949 continue, while the mean velocity of expansion remains practically the same as in previous years. [less ▲] Detailed reference viewed: 8 (1 ULg)The Spectrum of Nova DQ Herculis (1934) in 1947 and 1949.Swings, Polydore ; in Astrophysical Journal (1950), 110 Detailed reference viewed: 7 (4 ULg)The Spectra of the Wolf-Rayet Stars in the Region λλ 6500-8800.Swings, Polydore ; in Astrophysical Journal (1950), 111 The spectra of seven Wolf-Rayet stars have been observed in the region λλ 6500-8800. For the identifications, tables of predicted lines of C II-IV, O II-IV, and Si III and IV were prepared. All strong ... [more ▼] The spectra of seven Wolf-Rayet stars have been observed in the region λλ 6500-8800. For the identifications, tables of predicted lines of C II-IV, O II-IV, and Si III and IV were prepared. All strong emission lines are satisfactorily explained in the WC sequence; in the WN sequence, a fairly strong complex emission near λ 8240 remains unidentified. [less ▲] Detailed reference viewed: 8 (4 ULg)The Spectrum of Comet 19481.; Swings, Polydore in Astrophysical Journal (1950), 111 Eight spectrograms of Comet 19481, covering the range of heliocentric distances from 0.65 to 2.21 A.U., have been obtained. Sodium emission is observed at r = 0.73 and r = 0.79 A.U. At large heliocentric ... [more ▼] Eight spectrograms of Comet 19481, covering the range of heliocentric distances from 0.65 to 2.21 A.U., have been obtained. Sodium emission is observed at r = 0.73 and r = 0.79 A.U. At large heliocentric distances (r = 2.21) only CN and the λ 4050 group are observed. The CN bands show the usual complex structure due to the fluorescence excitation by solar radiation. The behavior of CH and that of CH2 are compared. Unidentified features are present within and between the Swan bands, as well as in the yellow-red region. [less ▲] Detailed reference viewed: 7 (3 ULg) |
||
