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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Was Wilhelm R?pke Really a Proto-Keynesian?te and oblate spheroids..It is shown that an asymmetry of the geometry of light scattering by non-spherical particles results in a component of the radiation pressure force . perpendicular to the wave-vector of incident light. For silicate spheroids, this component can exceed 20% of ∣.∣. For small m

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Was Wilhelm R?pke Really a Proto-Keynesian?he geometrical and dynamical structure of winds is also necessary to improve models of mass loss. The fact that mass loss from red giants may be episodic has been recognized early: for example, Sauner (1976) showed multiple absorption components in circumstellar absorption lines Ridgway (1981) analy

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Was Wilhelm R?pke Really a Proto-Keynesian? its effective temperature, .., starts to increase, which soon causes the mass loss rate to decrease significantly. When .. reaches about 30 000 K, the star eventually enters the planetary nebula (PN) phase. The transition from the AGB to the PN stage, believed to last a few thousand years, is calle

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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.

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ISO LWS Observations of Evolved Stars and Nebulaenfrared wavelengths by the Infrared Space Observatory (ISO) since its launch in November 1995. The results reported have been obtained mainly using ISO’s Long Wavelength Spectrometer (LWS; Clegg et al. 1996), but for some objects complementary spectra have also been obtained with the Short Wavelengt

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