The relation between molecular clouds and stellar kinematics

Details The relation between molecular clouds and stellar kinematics The relation between molecular clouds and stellar kinematics

Dec 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986ap%26ss.128..151p&link_type=abstract

(Universitaets-Sternwarte Jena, Jena Workshop on the Role of Dust in Dense Regions of Interstellar Matter, Georgenthal, East Ger

Astronomy and Astrophysics

Astronomy

Milky Way Galaxy, Molecular Clouds, Star Clusters, Star Formation, Stellar Motions, Black Holes (Astronomy), Early Stars, O Stars, Open Clusters, Stellar Systems

Scientific paper

The relation between molecular clouds, star clusters, and the stellar component of the galactic disk is investigated. According to Elmegreen (1985), bound stellar systems, e.g., open star clusters, can be formed from molecular cloud of mass equal to about 10,000 solar masses. A close encounter with a giant molecular cloud or massive black hole disrupts such stellar systems and forms superclusters. This explains why some open star clusters are so mass-deficient. Unbound stellar systems, e.g., expanding OB associations, are formed from molecular clouds of mass greater than about 10 to the 5th solar masses. When disruptive O-type stars appear, the star formation is halted, and the cloud is destroyed. An example of the relict of giant molecular cloud (GMC) disruption in the solar vicinity is Gould's belt. The velocity dispersion-versus-age relation is also investigated and explained as a consequence of gravitational scattering of stars on GMC, or massive black holes, or as due to recurrent transient spirals.

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