Two-Component Model for Chemical Evolution of the Galactic Disk

Chang, Ruixiang; Hou, J. L.; Shu, C. G.; Fu, C. Q.

doi:10.1142/9789812810830_0056

Cited by 20 publications

(35 citation statements)

References 50 publications

(76 reference statements)

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“…This conclusion has subsequently also been stressed by other authors (e.g. Portinari, Chiosi & Bressan 1998; Prantzos & Silk 1998; Chang et al 1999).…”

Section: Introductionsupporting

confidence: 69%

K dwarfs and the chemical evolution of the solar cylinder

Kotoneva¹,

Flynn²,

Chiappini³

et al. 2002

Monthly Notices of the Royal Astronomical Society

114

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K dwarfs have lifetimes older than the present age of the Galactic disc, and are thus ideal stars for investigating the chemical evolution of the disc. We have developed several photometric metallicity indicators for K dwarfs, based on a sample of accurate spectroscopic metallicities for 34 disc and halo G and K dwarfs. The photometric metallicities lead us to develop a metallicity index for K dwarfs based only on their position in the colour–absolute‐magnitude diagram. Metallicities have been determined for 431 single K dwarfs drawn from the Hipparcos catalogue, selecting the stars by absolute magnitude and removing multiple systems. The sample is essentially a complete reckoning of the metal content in nearby K dwarfs. We use stellar isochrones to mark the stars by mass, and select a subset of 220 of the stars, which is complete within a narrow mass interval. We fit the data with a model of the chemical evolution of the solar cylinder. We find that only a modest cosmic scatter is required to fit our age–metallicity relation. The model assumes two main infall episodes for the formation of the halo‐thick disc and thin disc, respectively. The new data confirm that the solar neighbourhood formed on a long time‐scale of the order of 7 Gyr.

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“…This conclusion has subsequently also been stressed by other authors (e.g. Portinari, Chiosi & Bressan 1998; Prantzos & Silk 1998; Chang et al 1999).…”

Section: Introductionsupporting

confidence: 69%

K dwarfs and the chemical evolution of the solar cylinder

Kotoneva¹,

Flynn²,

Chiappini³

et al. 2002

Monthly Notices of the Royal Astronomical Society

114

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show abstract

“…Chiappini et al 1997;Chang et al 1999;Alibés et al 2001). Chiappini et al 1997;Chang et al 1999;Alibés et al 2001).…”

Section: • Parallel Formationunclassified

The Origin of the Galaxy and Local Group

Bland‐Hawthorn

Freeman

Matteuccí

2014

Saas-Fee Advanced Course

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“…To create a modelled spectral energy distribution (SED) we apply the evolutionary synthesis modelling technique, considering that the SFH follows a determined distribution. For the purpose of this study, based on the inside-out model of galaxy formation, we assume that the SFR of the galaxy vary with time following a Gaussian distribution [11].…”

Section: Methodsmentioning

confidence: 99%

Isolated Galaxies versus Interacting Pairs with MaNGA

et al. 2015

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We present preliminary results of the spectral analysis on the radial distributions of the star formation history in both a galaxy merger and a spiral isolated galaxy observed with MaNGA. We find that the central part of the isolated galaxy is composed by older stellar population (∼2 Gyr) than in the outskirts (∼7 Gyr). Also, the time-scale is gradually larger from 1 Gyr in the inner part to 3 Gyr in the outer regions of the galaxy. In the case of the merger, the stellar population in the central region is older than in the tails, presenting a longer time-scale in comparison to central part in the isolated galaxy. Our results are in agreement with a scenario where spiral galaxies are built from inside-out. In the case of the merger, we find evidence that interactions enhance star formation in the central part of the galaxy.

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Two-Component Model for Chemical Evolution of the Galactic Disk

Cited by 20 publications

References 50 publications

K dwarfs and the chemical evolution of the solar cylinder

K dwarfs and the chemical evolution of the solar cylinder

The Origin of the Galaxy and Local Group

Isolated Galaxies versus Interacting Pairs with MaNGA

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