1998
DOI: 10.1002/asna.2123190504
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The G‐dwarf problem in the solar neighbourhood: a Lagrangian picture. II

Abstract: The current paper investigates how the empirical, G-dwarf metallicity distribution constrains simple, comoving models of chemical evolution. In doing this, the application of the models to a data sample, performed in a previous paper, is refined and extended. The key idea is that (i) different star formation rates with different mass spectra take place in different phases of evolution, i.e. contraction and equilibrium, and (ii) disk formation begins at a time t = T d and ends at t = T,, which marks the transit… Show more

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Cited by 6 publications
(25 citation statements)
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“…Accordingly, a one-to-one correspondence between stars of assigned age and metal content cannot be established as in the simple model (e.g., Caimmi 1997Caimmi , 1998. More precisely, it may be sketched as a series of segments with equal lenght and slope, but not aligned, except in the limit where all the regions are active and the current model reduces to a simple model.…”
Section: Theoretical Age-metallicity Relation and G-dwarf Metallicitymentioning
confidence: 93%
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“…Accordingly, a one-to-one correspondence between stars of assigned age and metal content cannot be established as in the simple model (e.g., Caimmi 1997Caimmi , 1998. More precisely, it may be sketched as a series of segments with equal lenght and slope, but not aligned, except in the limit where all the regions are active and the current model reduces to a simple model.…”
Section: Theoretical Age-metallicity Relation and G-dwarf Metallicitymentioning
confidence: 93%
“…Comoving models of chemical evolution have been exhaustively treated elsewhere by the author (e.g., Caimmi 1997Caimmi , 1998; and further references therein). For this reason, only what is relevant for the current attempt will be repeated here.…”
Section: Main Assumptionsmentioning
confidence: 99%
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“…Accordingly, the oxygen abundance within stars is monotonically increasing with time in the range ´Ø µ ´Ø µ ,in ½ ¾ , is (Caimmi 1998): …”
Section: 2 Inhomogeneous Modelsmentioning
confidence: 99%