I Feel, Therefore I Think

McDonald, Helen; Bennett, Jill; Alphen, Ernst van

doi:10.2307/20068471

Cited by 3 publications

(4 citation statements)

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“…While stars in the sample presented in Sloan et al (2010) are more metal rich than the models presented here, the two sources belonging to NGC 4372, analyzed in McDonald et al (2013), have a similar metallicity ([Fe/H]= −2.2), which offers the opportunity of a more detailed comparison. From the spectra, the authors argue that the two stars are oxygen-rich, and dusty.…”

Section: Carbon and Sic Dust In Low-mass Agbsmentioning

confidence: 68%

“…Fig.5 shows that some carbon-dust production is expected in these low-mass objects, provided that some extra mixing from the convective zones is adopted. This is however not in contrast with the fact that the two stars examined by McDonald et al (2013) are oxygen-rich, because even in case that a large extra mixing is used, the model achieve the C-star stage only in the lates evolutionary phases, while the surface remains oxygen-rich for most of the duration of the AGB phase.…”

Section: Carbon and Sic Dust In Low-mass Agbsmentioning

confidence: 97%

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Dust formation in the winds of AGBs: the contribution at low metallicities

Criscienzo¹,

Dell’Agli²,

Ventura³

et al. 2013

Monthly Notices of the Royal Astronomical Society

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We present new models for the evolution of stars with mass in the range 1M ⊙ M 7.5M ⊙ , followed from the pre-main-sequence through the asymptotic giant branch phase, until most of their envelope is lost via stellar winds. The metallicity adopted is Z = 3 × 10 −4 (which, with an α−enhancement of +0.4, corresponds to [F e/H] = −2). Dust formation is described by following the growth of dust grains of various types as the wind expands from the stellar surface.Models with mass M 3M ⊙ experience Hot Bottom Burning, thus maintaining the surface C/O below unity. Unlike higher Z models, the scarcity of silicon available in the envelope prevents the formation of silicates in meaningful quantities, sufficient to trigger the acceleration of the wind via radiation pressure on the dust grains formed. No silicate formation occurs below a threshold metallicity of Z = 10 −3 .Low-mass stars, with M 2.5M ⊙ become carbon stars, forming solid carbon dust in their surroundings. The total dust mass formed depends on the uncertain extent of the inwards penetration of the convective envelope during the Third Dredge-Up episodes following the Thermal Pulses. However, provided that a minimum abundance of carbon of X(C) ∼ 5×10 −3 is reached in the envelope, the results turn out to be fairly independent of the parameters used. Carbon grains have sizes 0.08 mum < a C < 0.12 µm and the total amount of dust formed (increasing with the mass of the star) isOur results imply that AGB stars with Z = 3×10 −4 can only contribute to carbon dust enrichment of the interstellar medium on relatively long timescales, > 300 Myr, comparable to the evolutionary time of a 3M ⊙ star. At lower metallicities the scarcity of silicon available and the presence of Hot Bottom Burning even in M< 2 M ⊙ , prevents the formation of silicate and carbon grains. We extrapolate our conclusion to more metal-poor environments, and deduce that at Z < 10 −4 dust enrichment is mostly due to metal condensation in supernova ejecta.

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Section: Carbon and Sic Dust In Low-mass Agbsmentioning

confidence: 68%

Section: Carbon and Sic Dust In Low-mass Agbsmentioning

confidence: 97%

Dust formation in the winds of AGBs: the contribution at low metallicities

Criscienzo¹,

Dell’Agli²,

Ventura³

et al. 2013

Monthly Notices of the Royal Astronomical Society

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“…Seni kontemporer adalah sebuah aliran yang menolak diinterpretasikan dalam disiplin aliran ekspresionis atau konseptualis. Karya-karya di jalur seni kontemporer menekankan keterlibatannya dengan ingatan dan tubuh melalui kesan panca indera terhadap gambaran yang mengharukan dalam kehidupan sehari-hari (Mc Donald, 2006).…”

Section: Karya Seni Dan Relevansi Dengan Perilaku Penikmat (Audience unclassified

Klasifikasi Prioritas Ketertarikan Perilaku Pengunjung Pameran Terhadap Karya Seni Rupa Kontemporer

Waryanti¹

2017

INVENSI

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Many elements are presented to visitors during an exhibition of contemporary art. These elements include the overaching concept of the exhibit (Ko), issues raised in the exhibition (Is), the name of the artist whose popularity attracts patrons (Na), and visual forms of the art itself (Vi). Using these four elements I compiled questions and interviewed patrons with various backgrounds in the arts. The goal was to find out these patron’s interest priorities; in other words, which aspects of the exhibit were of most interest to them as an observer. Previous literature on visitor behavior and social response at contemporary art exhibitions has been used as a base for this research. This study aims to highlight the different interest priorities as a visitor behaviour and audiens reception due to exhibition. I My respondences in this research is the exhibition visitors who had a background in art, but not necessarily in the discipline being exhibited. The results of this study will serve to determine the interest of art exhibition patrons, so that artists and curators can be made more aware of the gaps that exist between exhibit creation and viewer interest, and how those gaps can be better closed.

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“…For confirmation, we checked the bright outliers, indicated by red circles in Fig. 2, for proper motions in the USNO-B1.0 catalog (Monet et al 2003) and the NOMAD catalog (Zacharias et al 2005), although in many cases these are not fully conclusive (e.g., see McDonald et al 2013 for a similar approach to the bright AGB stars in NGC 4372). Once we are convinced that the star is a true non-member, the star is cleaned from the cluster photometry by subtracting its flux, based on the DAOPHOT PSF magnitudes, from the flux in the cluster aperture.…”

Section: Removing Foreground Starsmentioning

confidence: 99%

G2C2 – I. Homogeneous photometry for Galactic globular clusters in SDSS passbands

Vanderbeke

West

Propris

et al. 2013

Monthly Notices of the Royal Astronomical Society

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We present g and z aperture photometry for 96 Galactic Globular Clusters, making this the largest homogeneous catalog of photometry for these objects in the SDSS filter system. For a subset of 56 clusters we also provide photometry in r and i . We carry out comparisons with previous photometry as well as with the SDSS dataset. The data will be useful for a series of applications in Galactic and extragalactic astrophysics. Future papers will analyse the colourmetallicity relation, colour-magnitude diagrams, and structural parameters. The compilation of results based on this dataset will be collected in the Galactic Globular Cluster Catalog (G2C2).

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I Feel, Therefore I Think

Cited by 3 publications

References 0 publications

Dust formation in the winds of AGBs: the contribution at low metallicities

Dust formation in the winds of AGBs: the contribution at low metallicities

Klasifikasi Prioritas Ketertarikan Perilaku Pengunjung Pameran Terhadap Karya Seni Rupa Kontemporer

G2C2 – I. Homogeneous photometry for Galactic globular clusters in SDSS passbands

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