Titlebook: Dust and Molecules in Evolved Stars; Proceedings of an In Isabelle Cherchneff,Tom J. Millar Conference proceedings 1998 Springer Science+Bu

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Theodore Pelagidis,Michael Mitsopoulosof the interstellar UV field can initiate a complex photochemistry. These models use as input the abundances of parent species which are either set from observational data or from LTE abundances, which are valid in the photosphere, and which assume that the molecules pass through the inner layers of

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Osmosis

No Villainous Mother—The Life of Eva Larkinjects. The observations reveal that there is an observable chemical evolution in the neutral gas as a star evolves beyond the AGB, through the proto-PN and PN phases. Significant changes in the abundances of some key molecules (such as CS, CN, HCO., HCN, and HC.N) take place during the fast evolutio

衍生

No Villainous Mother—The Life of Eva Larkinved stars. Where can we expect circumstellar molecular spectra, why would we want to study these spectra, which molecules might be present, and what can we learn from these studies? We present an overview of reported detections, and discuss some of the results.

bromide

No Villainous Mother—The Life of Eva Larkinarbon-rich star with an oxygen-rich circumstellar envelope. The CO emission from both of these disks has a spike with a width near ~2 km s., indicating disk radii of 10. cm. The dust in such disks is therefore quite cold (near T ~ 50 K for the Red Rectangle) and may emit primarily at submillimeter w

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Wilhelm R?pke: Why He Was a Conservativeover the entire range observed for carbon Miras. The luminosities are calculated from a period-luminosity relation. Parameters derived are the distance, the dust mass loss rate and the ratio of silicon carbide to amorphous carbon dust. The total mass loss rate is derived from a modified relation bet

CLIFF

Wilhelm R?pke and American Conservatismture is not yet well established. This subject has been addressed by several authors and good fits of a large number of IRAS sources (chosen among the carbon stars exhibiting the SiC feature at about 11.3 pm) were obtained. In this work we use the same procedure on a limited number of objects, of th

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