The chemical evolution of the solar neighborhood. II - The age-metallicity relation and the history of star formation in the galactic disk

Details The chemical evolution of the solar neighborhood. II - The age-metallicity relation and the history of star formation in the galactic disk The chemical evolution of the solar neighborhood. II - The age-metallicity relation and the history of star formation in the galactic disk

Nov 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980apj...242..242t&link_type=abstract

Astrophysical Journal, Part 1, vol. 242, Nov. 15, 1980, p. 242-259.

Astronomy and Astrophysics

Astrophysics

516

Chemical Evolution, Galactic Evolution, Metallic Stars, Milky Way Galaxy, Star Formation, Abundance, Astronomical Models, Dwarf Stars, F Stars, G Stars, Scale Height, Star Formation Rate, Stellar Evolution

Scientific paper

The age-metallicity relation for the disk in the neighborhood of the sun is derived from four-color and H-beta photometry of a large sample of southern F dwarfs, analyzed in combination with theoretical isochrones. It is found that the mean metallicity of the disk increased by about a factor of five between 12 and 5 billion years ago and has increased only slightly since then. The star formation rate (SFR) for the disk as a function of time is obtained from the number count data, taking into account stellar evolution and the disk scale height corrections. The SFR which produces a metallicity distribution for the F stars consistent with the G dwarf data is one where the SFR has remained relatively constant over the lifetime of the disk. It is concluded that the disk has collapsed by about a factor of 6 perpendicular to the galactic plane during its lifetime, most of the collapse occurring 13 to 7 billion years ago.

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