The fragmentation of proto-globular clusters. I - Thermal instabilities

Details The fragmentation of proto-globular clusters. I - Thermal instabilities The fragmentation of proto-globular clusters. I - Thermal instabilities

Apr 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989apj...339..933m&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 339, April 15, 1989, p. 933-942. Research supported by NASA.

Astronomy and Astrophysics

Astrophysics

69

Astronomical Models, Fragmentation, Globular Clusters, Hydrodynamic Equations, Star Formation, Thermal Instability, Abundance, Gas Heating, Gravitational Collapse, Hydrogen

Scientific paper

The metal abundances among the stars within a typical globular cluster are remarkably homogeneous. This indicates that star formation in these systems was a globally coordinated event which occurred over a time span less than or comparable to the collapse time scale of the cluster. This issue is addressed by assuming that the fragmentation of a proto-globular cluster cloud proceeded in two steps. In the first step, thermal instability led to the rapid growth of initial fluctuations. This led to a large contrast in the dynamical time scales between the perturbations and the parent cloud, and the perturbations then underwent gravitational instabilities on short time scales. This process is modeled using one-dimensional hydrodynamic simulations of clouds both with and without external heat sources and self-gravity. The models include the effects of a non-equilibrium H2 abundance. The results indicate that fragmentation can occur on time scales significantly less than the dynamical time scale of the parent cloud.

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