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See detailHD 167362, an object similar to Campbell's Hydrogen Envelope Star
Swings, Polydore ULg; Struve, Otto

in Proceedings of the National Academy of Sciences of the United States of America (1940), 26

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See detailThe spectrum of RW Hydrae
Swings, Polydore ULg; Struve, Otto

in Proceedings of the National Academy of Sciences of the United States of America (1940), 26

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See detailThe spectrum of the companion of α Scorpii.
Struve, Otto; Swings, Polydore ULg

in Astrophysical Journal (1940), 92

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See detailThe nebular spectra of two slow novae, DQ Herculis and RT Serpentis.
Swings, Polydore ULg; Struve, Otto

in Astrophysical Journal (1940), 92

The spectrum of Nova Herculis has been measured in the region λλ 3200-6700, and many new lines have been identified. The character of the spectrum has not changed greatly since the observations by Adams ... [more ▼]

The spectrum of Nova Herculis has been measured in the region λλ 3200-6700, and many new lines have been identified. The character of the spectrum has not changed greatly since the observations by Adams and Joy in 1935-1936, but the increased separation between the two visual components of the Nova has now made it possible to observe separately the two spectra. The ionization seems to be identically the same in the two objects, but some differences in the structure of the lines was noticed. Spectra taken with the slit along the major axis of the elongated image show a marked depression between the two outside components of the emission lines, while at least the preceding component of the binary shows a fairly strong central component between the two outside components. The observations are sensitive to conditions of seeing, and it is not possible at this stage to unravel the true nature of the spectroscopic structure of the lines. The spectrum of Nova Serpentis, which had an outburst in 1909 and which is known to have developed abnormally slowly, was last described by Joy in 1931. Since that time the spectrum has undergone marked changes: the lines of [Fe III], which were strong in 1931, are very weak on our spectrogram. Instead, [Ne III], [Ne V], and [Fe VI] are strong, in addition to H, He I, He II, and [O III]. [less ▲]

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See detailSpectrographic observations of peculiar stars.
Swings, Polydore ULg; Struve, Otto

in Astrophysical Journal (1940), 91

1. The spectra of several absorption O-type stars showing vestiges of Wolf-Rayet emission have been investigated from λ 3300 to λ 6700. The absorption spectrum consists mainly of H, He II, He I,O III,O IV ... [more ▼]

1. The spectra of several absorption O-type stars showing vestiges of Wolf-Rayet emission have been investigated from λ 3300 to λ 6700. The absorption spectrum consists mainly of H, He II, He I,O III,O IV, N III, N IV, and Si IV. The emission lines show a P Cygni character and are confined to H, He I, and a few transitions of He II, N III, N IV, N V, C III, and Si IV. The location of the expanding shell giving rise to the emission and absorption lines is estimated. 2. The visual spectrum of P Cygni reveals strong Fe III lines originating from metastable levels (dilution effect). Lines of other elements show a peculiar selectivity of the emission lines. The spectra of three other P Cygni type stars (Z Canis Majoris, BD+47°3487, and BD+11°4073) are described, especially in connection with the phenomena arising in expanding shells. RY Scuti shows a strong system of forbidden [Fe III] lines, and the variations in the spectrum of this star are discussed. 3. The ultraviolet region of the spectrum of ξ Tauri shows several sets of absorption lines (H, He, and ionized metals) arising from the reversing layer and from various layers in the surrounding shell. The a5D - 4p5P0 multiplet of Fe III was the most conspicuous feature in the visual region of γ Cassiopeiae in March, 1940. New data are given for the spectra of several other stars with extended shells (MtW 143, HD 218393, HD 160529, and HD 190073). A group of stars showing forbidden [Fe II] lines is discussed (WY Geminorum, W Cephei, B 1985, B 5481, and HD 45677) ; and new [Fe II] multiplets are found in the ultraviolet region of these objects. 4. The spectra of four binary systems showing simultaneously an M-type spectrum and forbidden lines of high excitation are described in detail. The spectroscopic phenomena accompanying the recent outburst of Z Andromedae are discussed; the continuous absorption in the shell plays an important role in the relative intensities of the emission and absorption components of the P Cygni type lines. The two stars AX Persei and CI Cygni have very similar bright-line spectra, of which the nebular part shows a very high excitation; besides H, He I, and He II, the strongest lines are due to [Fe VII] and [Ne V], and there is good evidence in favor of [Fe X]. The temperature of the nucleus exciting these nebular lines must be of the order of 150,000°, or more. Another multiple object of lower excitation is R Aquarii, and new spectroscopic data show the occultation effect of the nebula by the TiO atmosphere of the late-type component. There is good reason to beUeve that the binary nature of a star stimulates the process of shell formation. [less ▲]

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See detailThe spectrum of NGC 6543 and its nucleus
Swings, Polydore ULg

in Astrophysical Journal (1940), 92

In the nebula NGC 6543 Bowen's fluorescence mechanism is absent, and the recombination process is especially efficient, giving relatively strong lines of C II, C III, and N III. The nucleus is a Wolf ... [more ▼]

In the nebula NGC 6543 Bowen's fluorescence mechanism is absent, and the recombination process is especially efficient, giving relatively strong lines of C II, C III, and N III. The nucleus is a Wolf-Rayet star showing lines of N IV and C IV of similar intensities; it is thus an object intermediate between the WN and WC sequences. [less ▲]

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See detailThe spectrum of P Cygni in the Region λ 3000-λ 3300
Swings, Polydore ULg; Struve, O.

in Publications of the Astronomical Society of the Pacific [=PASP] (1940), 52

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See detailThe spectrum of T Coronae Borealis
Swings, Polydore ULg; Elvey, C. T.; Struve, Otto

in Publications of the Astronomical Society of the Pacific [=PASP] (1940), 52

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See detailNew emission lines in Mira Ceti
Swings, Polydore ULg

in Publications of the Astronomical Society of the Pacific [=PASP] (1940), 52

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See detailA strong emission line of C III in HD 192639
Swings, Polydore ULg; Struve, Otto

in Publications of the Astronomical Society of the Pacific [=PASP] (1940), 52

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See detailA note on stars with nebulous absorption lines
Swings, Polydore ULg; Struve, Otto

in Publications of the Astronomical Society of the Pacific [=PASP] (1940), 52

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See detailThe Spectrum of µ Centauri
Swings, Polydore ULg; Elvey, C.-T.; Struve, Otto

in Publications of the Astronomical Society of the Pacific [=PASP] (1940), 52

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See detailBright lines of Fe II in the spectrum of HD 50138
Struve, Otto; Swings, Polydore ULg

in Publications of the Astronomical Society of the Pacific [=PASP] (1940), 52

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See detailTuniciers (2ème partie) : embryogénèse
Van Beneden, Édouard ULg; de Selys-Longchamps, Marc

Book published by J.-E. Buschmann (1940)

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