Metallicity and star formation history of globular clusters

Details Metallicity and star formation history of globular clusters Metallicity and star formation history of globular clusters

Mar 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993acaps..12..349z&link_type=abstract

Chinese Astronomy and Astrophysics (ISSN 0275-1062) Transl. of Acta Astrophysica Sinica, vol. 12, no. 4, 1992, p. 349-356., vol.

Astronomy and Astrophysics

Astrophysics

Globular Clusters, Metallicity, Star Formation, Astronomical Models, Star Formation Rate, Stellar Evolution, Stellar Mass

Scientific paper

Using population synthesis method, the star formation history in globular clusters has been studied. No single star formation mode with a constant star formation rate (SER) and an invariable initial mass function (IMF) can fit the observations of globular clusters. There are at least two stages of star formation: a pollution stage and a starburst stage. In the pollution stage, either the IMF is very peculiar (only form massive stars), or its SFR is so small that the low-mass stars form only a little. A starburst then follows to form most stars in the globular cluster. Within the framework of Fall and Rees' model, the collisions between warm clouds in the two phase medium may provide a suitable external cause to stimulate the starburst.

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