Formation and Evolution of Minerals in Accretion Disks and Stellar Outflows

Gail, H. P.

doi:10.1007/3-540-45840-9_2

Cited by 44 publications

(46 citation statements)

References 95 publications

(162 reference statements)

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“…(1) is solved for v. Since nearly all of the dust is formed in the region where Γ > 1, the solution for the flow structure only weakly depends on how v is determined in the region Γ < 1. This simplified procedure was already used in our preceding papers (Gail & Sedlmayr 1999;Ferrarotti & Gail 2001, 2002, 2003, and it allows a simple and efficient calculation of rather complex dustformation models.…”

Section: Velocity and Density Structurementioning

confidence: 99%

Composition and quantities of dust produced by AGB-stars and returned to the interstellar medium

Ferrarotti¹,

Gail²

2006

A&A

322

510

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The composition of the dust mixture and the amounts of dust returned into the interstellar medium during the evolution of low and intermediate mass stars on the AGB is calculated by simple models for dust-forming stellar winds with M-, S-, and C-star chemistry. These models consider the most abundant dust species formed in circumstellar dust shells, i.e. olivine-and pyroxene-type silicate grains and iron grains in the case of M-stars, iron grains in the case of S-stars, and carbon, SiC, and iron grains in the case of C-stars. The wind models are combined with calculations of synthetic AGB-evolution to consistently determine the variation of the dust injection rate into the interstellar medium from AGB-stars with initial mass and metallicity as the stars evolve along the AGB and change their chemical surface compositions due to repeated "dredge-up" episodes. Numerical results are presented for initial stellar masses from 1 to 7 M and for metallicities between Z = 0.001 and Z = 0.04, which can then be used to calculate chemical evolution models for the dust content of galaxies.

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Section: Velocity and Density Structurementioning

confidence: 99%

Composition and quantities of dust produced by AGB-stars and returned to the interstellar medium

Ferrarotti¹,

Gail²

2006

A&A

322

510

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“…Ferrarotti & Gail (2006) performed extensive calculations of dust formation by low-and intermediate-mass stars during their AGB evolution for a wide range of initial stellar masses and metallicities, making these models the most suitable for use in evolutionary dust models. Their work is based on detailed theoretical models of non-equilibrium dust condensation in stellar winds, developed in a series of earlier papers (Gail & Sedlmayr 1987Ferrarotti & Gail 2001Gail 2003). These studies consider the formation of a multicomponent dust mixture in stationary, dust-driven winds with O-, C-, and S-chemistries.…”

Section: Dust Formation By Low-and Intermediate-mass Starsmentioning

confidence: 99%

Dust input from AGB stars in the Large Magellanic Cloud

Zhukovska

Henning

2013

A&A

112

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Aims. The dust-forming population of AGB stars and their input to the interstellar dust budget of the Large Magellanic Cloud (LMC) are studied with evolutionary dust models with the main goals (1) to investigate how the amount and composition of dust from AGB stars vary over the galactic history; (2) to characterise the mass and metallicity distribution of the present population of AGB stars; (3) to quantify the contribution of AGB stars of different mass and metallicity to the present stardust population in the interstellar medium (ISM). Methods. We used models of the stardust lifecycle in the ISM developed and tested for the solar neighbourhood. The first global spatially resolved reconstruction of the star formation history of the LMC from the Magellanic Clouds Photometric Survey was employed to calculate the stellar populations in the LMC. Results. The dust input from AGB stars is dominated by carbon grains from stars with masses 4 M almost during the entire history of the LMC. The production of silicate, silicon carbide, and iron dust is delayed until the ISM is enriched to about half the present metallicity in the LMC. For the first time, theoretically calculated dust production rates of AGB stars are compared with those derived from infrared observations of AGB stars for the entire galaxy. We find good agreement within scatter of various observational estimates. We show that the majority of silicate and iron grains in the present stardust population originate from a small population of intermediate-mass stars consisting of only 4% of the total number of stars, whereas in the solar neighbourhood they originate from low-mass stars. With models of the lifecycle of stardust grains in the ISM we confirm the strong discrepancy between dust input from stars and the existing interstellar dust mass in the LMC reported previously.

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“…Condensation theory predicts that silicate growth can only proceed on nm-sized oxide seed nuclei [111]. While sub-grains (mostly carbides) have been observed in abundance in presolar graphite and SiC grains, oxides are generally absent within presolar silicate grains.…”

Section: Ancient Interstellar Dustmentioning

confidence: 99%

“…Many of these phases have narrow ranges of stability and may react to form other compounds as temperatures decrease before leaving the circumstellar environment. Amorphous silicates condense below about 800 K [111]. Amorphous silicates may anneal to crystalline phases upon heating to ~1000 K in a matter of hours to years, depending upon the composition and ambient temperature [111].…”

Section: Ancient Interstellar Dustmentioning

confidence: 99%