Derivation of the age-metallicity relation and initial mass function of stars in the solar neighbourhood

Details Derivation of the age-metallicity relation and initial mass function of stars in the solar neighbourhood Derivation of the age-metallicity relation and initial mass function of stars in the solar neighbourhood

Nov 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992a%26a...265..499r&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 265, no. 2, p. 499-503.

Astronomy and Astrophysics

Astrophysics

52

Metallicity, Solar Neighborhood, Stellar Evolution, Stellar Mass, Astronomical Models, Chemical Evolution, Dark Matter, Star Distribution

Scientific paper

The age-metallicity reaction (AMR) for the sun-like dwarf stars in the solar neighborhood has been derived here using the reasonably complete volume-limited data on the metallicity distribution of G-dwarfs from Pagel (1989) and the evolution of star formation rate (SFR) in the past from Soderblom et al. (1991), and compared with the existing AMRs. The SFR has also been corrected for the possible inflation of scale heights with age to obtain the actual variation of the star formation rate per unit area. The evolution of iron in the solar neighborhood has been computed using a simple closed model of chemical evolution and is shown to agree well with the AMR derived in the present work. Finally, we have used the SFR in the model proposed, as well as that from the Soderblom et al. (1991) sample to derive the initial mass function (IMF) of the local stars with due corrections for the effects of stellar multiplicity. We find that if we take into account the possible multiplicity of stars in the solar neighborhood, the mass function derived is such that we do not need to postulate the presence of any dark matter in the local disk.

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