2014
DOI: 10.5303/jkas.2014.47.6.219
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Astrophysics of Dusty Stellar Winds From Agb Stars

Abstract: Abstract:The main site of dust formation is believed to be the cool envelopes around AGB stars. Nearly all AGB stars can be identified as long-period variables (LPVs) with large amplitude pulsation. Shock waves produce by the strong pulsation and radiation pressure on newly formed dust grains drive dusty stellar winds with high mass-loss rates. IR observations of AGB stars identify various dust species in different physical conditions. Radio observations of gas phase materials are helpful to understand the ove… Show more

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Cited by 8 publications
(12 citation statements)
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References 65 publications
(90 reference statements)
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“…One thermal pulse every 10 4 -10 5 years that endures for a few hundred years is expected (Iben & Renzini 1983;Vassiliadis & Wood 1993). The chemical transition from O to C and superwind, which is induced by a thermal pulse, is known to make major effects on the dust envelopes around AGB stars (e.g., Groenewegen et al 1995;Suh 2014).…”
Section: Intoductionmentioning
confidence: 99%
See 1 more Smart Citation
“…One thermal pulse every 10 4 -10 5 years that endures for a few hundred years is expected (Iben & Renzini 1983;Vassiliadis & Wood 1993). The chemical transition from O to C and superwind, which is induced by a thermal pulse, is known to make major effects on the dust envelopes around AGB stars (e.g., Groenewegen et al 1995;Suh 2014).…”
Section: Intoductionmentioning
confidence: 99%
“…The dust formation temperature looks to be higher for the AGB stars with higher mass-loss rates (see Suh 2004). The dust size distribution for AGB stars could be a Gaussian distribution rather than a power law which is more relevant to interstellar dust (e.g., Kozasa et al 1984;Suh 2014).…”
Section: Formation and Growthmentioning
confidence: 99%
“…This phase of evolution is characterized by two nuclear burning shell of hydrogen and helium where hydrogen burning shell lies below the convective envelope and helium burning shell lies above the electron-degenerate core of carbon and oxygen, or for the most massive AGB stars a core of oxygen, neon, and magnesium [1]. This AGB stage is characterized by low surface effective temperatures (below 3000K) and intense mass loss (from10 −7 to 10 −4 M⊙yr −1 ) [2]. When the gas temperature drops to the sublimation temperature range, heavy elements in the mass outflow from a central star will condense to form dust .…”
Section: Introductionmentioning
confidence: 99%
“…AGB stars show characteristic spectral features from the central stars (identified by the optical spectra) or dust and gas envelopes (identified by the IR spectra or radio maser emission) and most AGB stars can be identified as LPVs (e.g., Kwon & Suh 2012;Suh 2014). …”
Section: Sample Of Agb Starsmentioning
confidence: 99%
“…Most AGB stars are longperiod variables (LPVs) which show large amplitude pulsations. The cool envelopes around AGB stars are believed to be the main site of dust formation (e.g., Suh 2014).…”
Section: Introductionmentioning
confidence: 99%