Titlebook: CNO Isotopes in Astrophysics; Proceedings of a Spe Jean Audouze Conference proceedings 1977 D. Reidel Publishing Company, Dordrecht,Holland

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https://doi.org/10.1007/978-3-662-66225-0e sole exception of the λ4232 line of .CH. which is seen in absorption against ζOph (Bortolot and Thaddeus, 1969; Vanden Bout, 1972). This single line together with rocket observations of the CO ultraviolet bands (Smith and Stecher, 1969) has provided our total knowledge of the relative abundance of

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Desinfektion, Hygiene und Infektionsschutz,ope ratios derived from observations reported up to August 1976. Except for the Orion Molecular Cloud, all H.CO ratios were obtained from the 1.-1. absorption line, at 4.8 GHz. The HC.N data of Churchwell et al. ((1976), ref. 7 in Table 1) were measured at 9 GHz. All other isotope results were obtai

鋼筆尖

https://doi.org/10.1007/978-3-662-68674-4he high vapor pressure of CO may cause a preferential loss of .C from the gas due to freezing onto dust grains. The .c/.c ratio for the carbon in the gas is then raised by factors ～ 2 to 4. Fractionation of deuterium is also discussed since the proposed process is similar to the carbon isotope excha

Bronchial-Tubes

War, Culture and Society, 1750–1850cumulated at the present on these elements focusing in particular on their isotopic composition. Study of isotopes is indeed most profitable in the sense that they are less affected than elements by chemical fractionation processes although such processes can be considered and be important (see e.g.

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https://doi.org/10.1007/978-3-663-01782-0 masses and ages, even for a fixed initial metal-abundance. Moreover, comparison of a given star with theoretical models may be rendered somewhat uncertain by errors in parrallax or other criteria of absolute magnitude.