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See detailThe Bands of CH and CN in Stellar Spectra
Swings, Polydore ULg; Struve, Otto

in Physical Review (1932), 39

The upper limit of visibility in the spectral sequence of the CH band at λ4300 is found to be F8 (temperature about 6500°K). This value is considerably lower than has been adopted heretofore (classes F2 ... [more ▼]

The upper limit of visibility in the spectral sequence of the CH band at λ4300 is found to be F8 (temperature about 6500°K). This value is considerably lower than has been adopted heretofore (classes F2 to A0; temperatures 7900° to 13000°K). The region occupied by the CH band is very rich in strong atomic lines and it is therefore not permissible to consider the general aspect of the Fraunhofer "G-band": the total intensity of the atomic lines greatly exceeds that of the molecular lines. The limit of visibility of the CN band at λ4200 is found to be at F8, in agreement with former estimates. The simultaneous disappearance of CH and CN, having heats of dissociation of 110 and 210 k cal/mol respectively, may be explained by the great abundance of H in stellar atmospheres. [less ▲]

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See detailLes bandes moléculaires dans les spectres stellaires
Swings, Polydore ULg

Book published by Hermann (1932)

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See detailOn the interpretation of the emission lines in stars of early spectral class
Struve, Otto; Swings, Polydore ULg

in Astrophysical Journal (1932), 75

The emission-line spectra.-The presence of bright Fe II in the spectra of Be stars suggests that lines of other elements requiring similar conditions of excitation may also be present. A search in the ... [more ▼]

The emission-line spectra.-The presence of bright Fe II in the spectra of Be stars suggests that lines of other elements requiring similar conditions of excitation may also be present. A search in the spectra of several stars yielded definite evidence of the presence of Mg II and Si II; Sc II, Cr II, and Ni II are probably present; forbidden Fe II is uncertain. No lines belonging to Ti II coµld be identified, with certainty. The width of the bright line Mg II 4481 greatly exceeds those of the emission lines of H, and in one star the lines of Fe II are definitely wider than those of H. Attributing the origin of the bright lines to a rotating shell of gas, and neglecting support by radiation pressure, we find that the effective distance of Mg II from the center is about seven times the radius of the star, while that of H is ten times the radius of the star. A rough computation of the density of the shell gives 2.5 x 10-13 gr/cm3. The bright lines of Mg II and of Si II are always weak. He I and Ti II are rarely seen in emission. Classification of bright-line spectra.-The published data on Be and Oe stars were collected and arranged according to the Harvard spectral class as derived from the absorption lines. The character of the emission lines shows a definite progression with spectral class. The degrees of effective excitation of the bright and dark lines are not very different in the Oe's but they differ by more than one spectral class in the Be's. There is relatively little dispersion within any given spectral subdivision. This would indicate, on the rotational hypothesis, that the product of the density of the shell and the dilution factor is approximately constant within a given subdivision, but that it varies as a function of spectral type. A new Be star.-Data are given for the Be star 60 Cygni (α 20h57m7 δ +45°46'), which has variable hydrogen lines. Variations in the spectra of Be stars.-Variations in the hydrogen lines of 31 Pegasi (α 22h16m6 δ +11°42') are described. The Be star 31 o Aquarii (α 21h58m1 δ -2°38') is found to have broad and hazy absorption lines of He I and Mg II, and sharp and narrow lines of Fe II. The latter are probably variable. This star is similar to the Be star Є Capricorni; and the suggestion is advanced that the hazy lines are broadened by rotation, while the narrow lines originate through absorption in the same rotating gaseous shell which is believed to give rise to the bright hydrogen lines and to their narrow central absorptions. The spectrum of 17 Leporis.-This spectrum seems to be related to spectra of the P Cygni type : 17 Leporis has bright Hβ in the normal position, accompanied by a strong absorption line on its violet side. Preliminary measurements of one plate give: Mg II +14 km/sec, Fe II and Ti II -64 km/sec, H -93 km/sec. The rotational hypothesis of the origin of bright lines.-A summary is given in support of the hypothesis that the bright lines originate in a rotating shell or ring of gas, and that the dispersion in line widths is mainly due to the effect of inclination. Objections to the rotational hypothesis are discussed and found not to be of a sufficiently serious nature to outweigh the positive evidence. The rotational hypothesis is adopted as the one which fits the observed facts better than any other theory thus far proposed. [less ▲]

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See detailMinor contributions and notes: an absorption line of C IV in stellar spectra
Mack, J.-E.; Swings, Polydore ULg; Struve, Otto

in Astrophysical Journal (1932), 76

An absorption line at λ 4658.41, observed in O-type stars, is probably identical with C IV 4658.64. This line has the distinction of requiring the greatest energy of excitation of any line yet observed in ... [more ▼]

An absorption line at λ 4658.41, observed in O-type stars, is probably identical with C IV 4658.64. This line has the distinction of requiring the greatest energy of excitation of any line yet observed in stellar absorption spectra. [less ▲]

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See detailThe bands of CH and CN in stellar spectra
Swings, Polydore ULg; Struve, Otto

in Physical Review (1932), 39(1), 142-150

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See detailSur les ds2 d'Espace-Temps contenant des termes en dt
Swings, Polydore ULg

in Bulletin de la Société Royale des Sciences de Liège (1932), 11

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See detailSur l'existence d'isotopes de Se et de Te, déduite de l'examen des multiplets de résonance de Se2 et de Te2
Swings, Polydore ULg; Cambresier, Y.

in Bulletin de la Classe des Sciences. Académie Royale de Belgique (1932), XVIII(5), 419-421

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See detailOn the interpretation of the emission lines in stars of early spectral class
Struve, Otto; Swings, Polydore ULg

in Astrophysical Journal (1932), LXXXV(3), 161-184

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See detailOn the behaviour of the bands of CH and CN in the spectrum of Delta Cephei
Swings, Polydore ULg

in Monthly Notices of the Royal Astronomical Society (1932), 92(2), 140-147

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See detailRemarque sur le spectre de résonance de la vapeur diatomique de Bismuth
Swings, Polydore ULg

in Bulletin de la Société Royale des Sciences de Liège (1932), (6), 1-3

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See detailQuelques considérations à propos des bandes ultra-violettes de CN dans les spectres stellaires
Swings, Polydore ULg

in Bulletin de la Société Royale des Sciences de Liège (1932), (3), 77-81

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See detailQuelques considérations déduites du spectre de résonance de la vapeur diatomique de tellure
Swings, Polydore ULg; Pierard, J.

in Bulletin de la Société Royale des Sciences de Liège (1932), (5), 109-114

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See detailLa fluorescence des vapeurs
Swings, Polydore ULg

in Revue Générale des Sciences Pures et Appliquées (1932), 43(juillet), 1-24

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See detailSur les bandes de CH et CN dans les étoiles des clases de F0 A G5
Swings, Polydore ULg

in Association Française pour l'Avancement des Sciences (Ed.) Compte-rendu de la 56e session, Bruxelles 1932 (1932)

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See detailSur de nouveaux verres très transparents aux ultra-violets
Swings, Polydore ULg; Gilard, P.

in Association Française pour l'Avancement des Sciences (Paris) (Ed.) Compte-rendu de la 56e session, Bruxelles 1932 (1932)

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See detailLes spectres de résonance et les isotopes
Swings, Polydore ULg

in Association Française pour l'Avancement des Sciences (Ed.) Compte-rendu de la 56e session, Bruxelles 1932 (1932)

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See detailLa vivisection
Duesberg, Jules ULg

Speech (1932)

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See detailAction de la fibrillation des ventricules sur le rythme des pulsations auriculaires du cœur du chien
Fredericq, Léon ULg

in Archives Internationales de Physiologie (1932), XXXV

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See detailAction de la fibrillation des ventricules sur le rythme des pulsations auriculaires du cœur du chien
Fredericq, Léon ULg

in Bulletin de l'Académie Royale de Médecine de Belgique (1932), XXII(4), 283

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