Titlebook: Mass-Losing Pulsating Stars and their Circumstellar Matter; Observations and The Y. Nakada,M. Honma,M. Seki Book 2003 Springer Science+Busi

人造

Stellar Sources in the Isogal Intermediate Bulge Fieldsnction and the mass-loss rates. A large fraction of the detected sources at 15 . are AGB stars above the RGB tip, a number of them show an excess in ([7]-[15])o and (K.-[15])o colors, characteristic of mass-loss. The latter, especially (K.-[15])o, allow estimation of the mass-loss rates (.) and show their distribution in the range 10. to 10. M./yr

故意钓到白杨

GAIA: AGB Stars as Tracers of Star Formation Histories in the Galaxy and Beyondt numbers of AGB stars in the Galaxy and beyond. Reliable ages of AGB stars can be determined to distances of ~200 kpc in a wide range of ages and metallicities, allowing star formation histories to be studied in a diversity of astrophysical environments

下船

kyphoplasty

Regular and Irregular Pulsations of Luminous Blue Variablesing through the stellar atmosphere. Ballistic motions of the outermost layers on the dynamic time scale of the atmosphere are interrupted by strong compressional shock waves. The deposition of energy and momentum leads to atmospheric stratifications that differ significantly from what prevails if hydrostatic stratification is assumed

Endearing

Period Evolution in Mira Variablesongest period Miras. In the case of R Hya, the period change was accompanied by a dramatic change in mass-loss rate, consistent with the mass-loss formalism of Vassiliadis & Wood. Their formalism then predicts that the mass-loss rates of the longest period Miras (. > 400days) may fluctuate by a factor of 2-3 over time scales of a century

黄油没有

Ceramic

Time Dependent Modelling of Mass Loss on the AGB .*) that should enable to determine when this instability takes place. Also, I present first results of calculations that follow the outflow on a timescale longer than that of the mass loss modulation (which is typically of the order of a hundred years). This enables to study the effect of stellar evolution on the wind

陶醉

Asymmetric Mass-Loss on the AGB: Examples from IRAS Datas of bi- or quadru-polar shape and will, due to their huge dimensions, probably have started to form already in the AGB phase. If so, then the mass-loss in the AGB phase is not spherically symmetric in a number of cases

pacifist

0067-0057 by the deadline. However, this time, thanks to the punctuality of all the participants, we have this excellent volume for the workshop on mass­ losing pulsating stars and their circumstellar matter prepared in time. Almost all of the oral presentations including the summary are collected in this vol

Adjourn