Late Stages of Stellar Evolution by W. David Arnett (auth.), R. J. Tayler, J. E. Hesser (eds.)

By W. David Arnett (auth.), R. J. Tayler, J. E. Hesser (eds.)

lAD Symposium No. sixty six used to be held in Warsaw from September tenth to September twelfth 1973, in reference to the extreme basic meeting of the lAD. It used to be prepared through lAD Symposium No. 35 and the clinical establishing Committee con­ sisted of A. G. Massevitch (Chairman), A. V. Tutukov (Secretary), H. M. van Horn, N. Dallaporta, J. P. Ostriker, B. Paczynski, G. Ruben, E. Schatzman, R. J. Tayler and A. Weigert. This quantity comprises the entire texts of the entire invited papers offered on the Symposium, except that added by means of R. P. Kraft, that is released in summary since it is showing in complete somewhere else. furthermore the quick communications given on the Symposium are released in summary. i tried to take down all the dis­ cussion because it happened and all individuals to the dialogue have been requested to supply copies in their feedback. From those assets an edited model of the dialogue has been produced. because the ultimate model has no longer been visible by way of the members, I can be held answerable for all mistakes. At Warsaw, many of the brief communications didn't instantly persist with the invited paper to which they referred. within the revealed model they and any dialogue on the subject of them are put within the most reasonable place. A small variety of brief communications, which have been circulated in summary at Warsaw yet that have been no longer added orally, also are integrated within the released version.

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We shall consider mainly the observational evidence for slow mass loss, and the alternative schemes for causing it. We shall also consider the observed mass loss in planetary nebulae, which may be caused this way, but not supernova or nova explosions. Thus we are left to consider, (i) radiation pressure driven winds, which have been discussed for red giants by Weymann (1962), Hoyle and Wickramasinghe (1962), and Gehrz and Woolf (1971). Then there are travelling waves (ii) which should only be important for pulsating stars, and can so be observationally distinguished.

Biermann (1968) investigated the stability of shell burning in Red Giants, with the result that the shells seem to be stable. Recently Richstone (1973) has studied stellar models near and during the onset of helium flash, and he found that all models investigated which were spherically stable were also stable with respect to non-spherical perturbations. Some flash models were unstable but the e-folding time of the non-spherical instability was longer than the e-folding time of the spherical instability.

The broken lines indicate the two shell sources eating outward. In intervals of about 4000 years thermal pulses occur forming short-living convective zones (vertical lines above the helium burning shell) which approach the hydrogen burning shell. The Scalo-U1rich plume mixing is supposed to occur as soon as the top of such a convective zone penetrates into the hydrogen burning shell. CIRCULATION AND MIXING 35 occur in an evolved star if carbon enriched material is brought up into a hydrogen rich outer region.

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