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Molecular dust precursors in envelopes of oxygen-rich AGB stars and red supergiants

Published online by Cambridge University Press:  30 December 2019

Tomasz Kamiński Open the ORCID record for Tomasz Kamiński [Opens in a new window]
Tomasz Kamiński*
Affiliation:
Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 Submillimeter Array Fellow, email: tkaminsk@cfa.harvard.edu
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Abstract

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Condensation of circumstellar dust begins with formation of molecular clusters close to the stellar photosphere. These clusters are predicted to act as condensation cores at lower temperatures and allow efficient dust formation farther away from the star. Recent observations of metal oxides, such as AlO, AlOH, TiO, and TiO2, whose emission can be traced at high angular resolutions with ALMA, have allowed first observational studies of the condensation process in oxygen-rich stars. We are now in the era when depletion of gas-phase species into dust can be observed directly. I review the most recent observations that allow us to identify gas species involved in the formation of inorganic dust of AGB stars and red supergiants. I also discuss challenges we face in interpreting the observations, especially those related to non-equilibrium gas excitation and the high complexity of stellar atmospheres in the dust-formation zone.

Keywords

stars: AGB and post-AGBcircumstellar matterstars: mass lossstars: windsoutflowsdustextinctionISM: molecules
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S343: Why Galaxies Care About AGB Stars: A Continuing Challenge through Cosmic Time , August 2018 , pp. 108 - 118
Copyright
© International Astronomical Union 2019 

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