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- W92215570 abstract "The AGB terminates with an episode of mass loss lasting a few times 10 years. The mechanism for this mass loss is pulsation combined with radiation pressure on grains for most stars with metallicity greater than about 30% of solar. The mass loss rate increases very steeply with increasing luminosity and radius and decreasing mass. The mass loss rate (and in some cases also the outflow velocity) on the AGB is modulated by (a) shell flash cycles and (b) an as-yet unidentified mechanism with a timescale of decades to centuries. The mechanism for AGB mass loss ceases to be effective when the envelope mass becomes small enough that the star begins to shrink. At the same time, a planet or low-mass companion may spin up or distort the envelope when Menv is less than about ten times the mass of the companion. The interaction of the envelope and any close body provides a natural mechanism for an event that would give rise to an asymmetric proto-planetary nebula inside a spherically symmetric distribution of material. In this review, we describe what is now reliably known about the events ending the AGB evolution of intermediate mass stars, and discuss some of the areas of uncertainty most relevant to the formation of APN. Mass loss on the asymptotic giant branch (AGB) sets the stage for the emergence of planetary nebulae. Empirical mass loss laws, such as Reimers’ relation Ṁ ∝ LR/M , have been widely used in modeling. Theoretical computations of the mass loss process yield mass loss laws that are much more sensitive to stellar parameters. One way to test these laws is to look at their implications for observable quantities such as direct determination of mass loss rate vs. stellar parameters, period vs. luminosity for Miras, initial vs. final mass relations, and the mass functions of the central stars of planetary nebulae and of white dwarfs. In what follows, we demonstrate that observed correlations between mass loss rates and combinations of stellar parameters may not be directly translated into mass loss laws useful for stellar evolution, but that they do, nonetheless, contain very valuable information about the mass loss process that ends the AGB. In the process, we demonstrate that most commonly used core mass luminosity relations cannot be correct." @default.
- W92215570 created "2016-06-24" @default.
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- W92215570 date "2004-07-01" @default.
- W92215570 modified "2023-09-24" @default.
- W92215570 title "Mass Loss at the Tip of the AGB" @default.
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