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See detailCometary spectra (Council report on the progress at astronomy)
Swings, Polydore ULg

in Monthly Notices of the Royal Astronomical Society (1943), 103

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See detailThe physical chemistry of comets
Swings, Polydore ULg

in Popular Astronomy (1943), 51

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

in Astrophysical Journal (1943), 98

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See detailFluorescence in astronomy
Swings, Polydore ULg

in Leaflet - Astronomical Society of the Pacific (1943), 4(175), 192-198

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See detailCometary emission spectra in the Visual Region.
Swings, Polydore ULg; McKellar, A.; Minkowski, R.

in Astrophysical Journal (1943), 98

A list of wave lengths of the emission features occurring in the region λ > 4800 has been compiled partly on the basis of previously published data but mainly from measurements of spectrograms of the ... [more ▼]

A list of wave lengths of the emission features occurring in the region λ > 4800 has been compiled partly on the basis of previously published data but mainly from measurements of spectrograms of the recent bright comets 1940c and 1942g obtained at the McDonald, the Mount Wilson, and the Dominion Astrophysical observatories. It is indicated that certain of the more prominent features behave, with respect to the comet's heliocentric distance, as emissions from polyatomic molecules would be expected to do. Comparison of the cometary spectrum with that of an oxyammonia flame leads to the suggested identification of a number of the emission features, among them the strong "λ 6300 group," as due to a dissociation product of ammonia, probably NH2. [less ▲]

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See detailThe spectrum of PLEIONE.
Struve, Otto; Swings, Polydore ULg

in Astrophysical Journal (1943), 97

The radial velocity of Pleione shows oscillations with a range of 10 km/sec and a period of about four months. The mean velocity is +5.5 km/sec. The spectrum of the shell, first discovered by McLaughlin ... [more ▼]

The radial velocity of Pleione shows oscillations with a range of 10 km/sec and a period of about four months. The mean velocity is +5.5 km/sec. The spectrum of the shell, first discovered by McLaughlin and Mohler in 1938, has gradually become stronger and now resembles the metallic spectrum of α Cygni. Dilution effects are conspicuous in the weakness of Mg II and Si II. Among the lines of ions having metastable lower levels, Ni II and Fe II became conspicuous in 1940, Ti II in 1941, and Mn II in 1942. This order of development is not consistent with the ordinary theory of ionization, and its explanation must be sought in the conditions of excitation of the metastable levels in the shell. The central intensities of the cores of the H lines are about 10 per cent—roughly one-half or one-third of the central intensities of the corresponding lines in α Cygni. This is explained as a consequence of the reduced re-emission which is thrown back within the shell into the emerging beam of radiation from the star. The metallic lines on the violet side of the Balmer limit and between the higher members of the series are relatively much stronger than in α Cygni. This is due to the semitransparency of the shell, on the one hand, and to the absence of Stark effect wings in the shell, on the other. [less ▲]

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See detailThe spectrum of Comet Whipple 2 (1942f)
Swings, Polydore ULg; Struve, Otto

in Publications of the Astronomical Society of the Pacific [=PASP] (1943), 55

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See detailForbidden lines of ionized nickel in the spectra of bright-line stars
Swings, Polydore ULg

in Publications of the Astronomical Society of the Pacific [=PASP] (1943), 55

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See detailAndré Vésale
Fredericq, Léon ULg

Book published by M. Hayez (1943)

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