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

巫婆

貧窮地活

Modeling the Long-Term Evolution of Dusty Outflows of AGB-Starss (typically 10. to 10. M.yr.) dominates over nuclear burning and finally terminates the AGB evolution. It is now generally accepted that the mechanism responsible for the high mass loss rates during the AGB evolution is based on the efficiency of . Shock waves generated by Mira-type stellar pulsati

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Observations of Shells Around , Cep & CRL2688, and about Episodic Mass Losshe 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

RACE

IR-Colors for Models of Post-AGB Evolution 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

Kindle

Variation of Silicate Dust Features with Phasen 8/95 & 4/97. With these data, we are attempting to ascertain the relationship of dust formation to optical period. Our ultimate goal is to determine what conditions lead to dust formation and destruction in these environments, and whether or not an evolutionary sequence can be inferred for AGB sta

歪曲道理

Molecules in Envelopes around AGB-Starsnt targets for the study of molecular formation processes. This review presents a compilation of estimated molecular abundances, discusses the uncertainties involved in their estimate, and makes some comparisons with theoretical predictions.

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樂章

Evocative

No Villainous Mother—The Life of Eva Larkinases with radius from ≤ 0.1 to ≤ 1.0 m. kg.. Comparison with laboratory studies suggests that small crystalline grains are formed near the star and are annealed into astronomical silicates at larger distances.