Abstract
AbstractA major role to the understanding of the chemical evolution of the Galaxy is played by studies of stellar chemical abundance distribution. In the last years, there has been an increase in the number of spectroscopic surveys of late-type stars. Classical problems on the chemical evolution of the Galaxy, such as the G dwarf problem and the age-metallicity relation, can be reinvestigated with better accuracy. We present a chemical abundance survey of 325 solar neighborhood G dwarfs stars situated within 25 pc from the Sun. We reinvestigate classical observational constraints, namely the metallicity distribution, using a number of chemical elements (Na, Si, Ca, Ni, Fe and Ba) as metallicity indicators. The abundance probability density function for each of the surveyed element was derived using a Gaussian kernel estimator. We have found mean values of −0.11, −0.14, −0.07, −0.05, −0.16 and −0.12 dex for the [Fe/H], [Na/H], [Si/H], [Ca/H], [Ni/H] and [Ba/H] pdfs, respectively. We also show that abundance distributions having higher mean values have smaller dispersion, in contradiction to the predictions of the Simple Model with Delayed Production. We discuss this result in the context and present an alternate explanation for this pattern.
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