Formation of globular clusters from gas in large-scale unorganized motion in galaxies

Details Formation of globular clusters from gas in large-scale unorganized motion in galaxies Formation of globular clusters from gas in large-scale unorganized motion in galaxies

Feb 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...404..144k&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 404, no. 1, p. 144-161.

Statistics

Computation

51

Globular Clusters, Interstellar Gas, Magellanic Clouds, Milky Way Galaxy, Stellar Evolution, Abundance, Andromeda Galaxy, Computational Astrophysics, Dynamical Systems, Gravitational Effects, Stellar Mass

Scientific paper

From dynamical data on interstellar gas and globular clusters with ages of 5 x 10 exp 6 - 10 exp 10 yr in the Magellanic Clouds, it is claimed that globular clusters may be generated at any time in any galaxy, if interstellar gas clouds are in large-scale unorganized motion with velocity of more than 50-100 km/s and they collide with each other to make strong local shock compressions. Dynamical and optical characteristics of globular clusters are explained to be consistent with this mechanism in the Galaxy, the Magellanic Clouds, M31, M33, M82, M87, NGC 1275, and other nearby galaxies. Theories are surveyed to produce a grand scenario that (1) the minimum mass of the Jeans gravitational instability is 10 exp 4 - 10 exp 6 solar masses for gas compressed by collision of clouds with velocity of 50-100 km/s or greater, (2) low-mass stars are more numerously and more quickly formed near the protoglobular cluster center, and (3) this stellar system is gravitationally stable against the blow-out of gas by newborn stars and/or by supernovae, which results in the delayed appearance of the cluster formation.

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