Titlebook: Mass Loss and Evolution of O-Type Stars; P. S. Conti,C. W. H. Loore Book 1979 International Astronomical Union 1979 spectroscopy.star.stel

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C IV Resonance Line Profiles in O Stars1 film with a 15 cm aperture objective-prism telescope. everal hundred early-type stars wer observed in the vicinity of 1550 Å with a resolution between 3 and 4 Å, as well as thousands of stars at longer wavelengths and correspondingly lower resolution. An atlas of spectra for types O4 to B5 is illu

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Winds in Hot, Subluminous Starst only do the young, massive OB stars (the subjects of our discussion in this symposium, so far) undergo high-velocity mass-loss, but so also do hot evolved, solar mass stars, among them the central star of planetary nebulae. In this talk, I would like to show ultraviolet spectra of two central star

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Analysis of UV Spectrophotometric Observations for O-type Stars Measured with Copernicus” (Snow and Jenkins 1976) have been used to try to separate, by means of simple diagrams, O-type stars belonging to different luminosity classes and having different temperatures. The ESA catalogue gives absolute fluxes for 43 O-type stars, mostly reddened, with a spectral r

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G. Hammerschlag-Hensbergeto gases, liquids, liquid crystals and solids (including polymers). Biochemists use it routinely for determining the structures of peptides and proteins, and it is also widely used in medicine (where it is often called MRI, Magnetic Resonance Imaging). With the advent of spectrometers operating at v

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Carlo Morossi,Roberto Stalio,Lucio Crivellarion polymerization of 1,3-butadiene produces.-1,4-,.-1,4-, syndio-1,2-, and iso-1,2-polymers which are obtained selectively by choosing the catalysts and the reaction conditions. Lanthanides catalyze polymerization of 1,3-butadiene to produce the.-1,4-polymer with excellent selectivity. The lanthanoc

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