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Wind Acceleration in AGB Stars: Solid Ground and Loose Ends
Uppsala University, Disciplinary Domain of Science and Technology, Physics, Department of Physics and Astronomy, Theoretical Astrophysics.
2015 (English)In: Why Galaxies Care About AGB Stars III: A Closer Look In Space And Time, ASTRONOMICAL SOC PACIFIC , 2015, Vol. 497, 333-343 p.Conference paper (Refereed)Text
Abstract [en]

The winds of cool luminous AGB stars are commonly assumed to be driven by radiative acceleration of dust grains which form in the extended atmospheres produced by pulsation-induced shock waves. The dust particles gain momentum by absorption or scattering of stellar photons, and they drag along the surrounding gas particles through collisions, triggering an outflow. This scenario, here referred to as Pulsation Enhanced Dust-DRiven Outflow (PEDDRO), has passed a range of critical observational tests as models have developed from empirical and qualitative to increasingly self-consistent and quantitative. A reliable theory of mass loss is an essential piece in the bigger picture of stellar and galactic chemical evolution, and central for determining the contribution of AGB stars to the dust budget of galaxies. In this review, I discuss the current understanding of wind acceleration and indicate areas where further efforts by theorists and observers are needed.

Place, publisher, year, edition, pages
ASTRONOMICAL SOC PACIFIC , 2015. Vol. 497, 333-343 p.
National Category
Astronomy, Astrophysics and Cosmology
URN: urn:nbn:se:uu:diva-294841ISI: 000371098100067OAI: oai:DiVA.org:uu-294841DiVA: diva2:933270
Conference on Why Galaxies Care About AGB Stars III: A Closer Look in Space and Time, JUL 28-AUG 01 2014, Univ Vienna, Vienna, AUSTRIA
Available from: 2016-06-03 Created: 2016-05-27 Last updated: 2016-06-03Bibliographically approved

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Hofner, Susanne
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