1997
DOI: 10.1002/asna.2113180606
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The G‐dwarf problem in the solar neighbourhood: a Lagrangian picture

Abstract: Recent data on the empirical metallicity distribution of G dwarfs in the disk solar neighbourhood are fitted in two different ways. We use an extended Poisson distribution in the limit where the probability of star formation is small, and a Gauss distribution in the limit where a large number of physical variables is required to determine stellar metal abundance. Both are found to reproduce the data at the same (acceptable) extent, with a slight preference for the former. The empirical, differential metallicit… Show more

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Cited by 6 publications
(25 citation statements)
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“…In fact, by "comoving model" we mean the chemical evolution of a volume comoving with the contraction. It has been shown in recent attempts that a generalized Schmidt star formation law, in the light of closed, comoving models, is consistent with observations related to both other galaxies (Caimmi 1995(Caimmi , 1996 and the solar neighbourhood (Caimmi 1997).…”
Section: Introductionsupporting
confidence: 74%
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“…In fact, by "comoving model" we mean the chemical evolution of a volume comoving with the contraction. It has been shown in recent attempts that a generalized Schmidt star formation law, in the light of closed, comoving models, is consistent with observations related to both other galaxies (Caimmi 1995(Caimmi , 1996 and the solar neighbourhood (Caimmi 1997).…”
Section: Introductionsupporting
confidence: 74%
“…As simple, comoving models assume instantaneous recycling, the comparison with observations must be related to oxygen instead of iron (see e.g., Pagel 1989;Wang & Silk 1993;Caimmi 1997). To this aim, we use the empirical fit (e.g., Pagel 1989;Prantzos & Aubert 1995): according to a currently accepted approximation (e.g., Malinie et al 1993):…”
Section: T H E G-dwarf Metallicity Distributionmentioning
confidence: 99%
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