ISSN:
1572-946X
Keywords:
High Velocity Clouds
;
Star formation
Source:
Springer Online Journal Archives 1860-2000
Topics:
Physics
Notes:
Abstract We simulated collisions of High Velocity Clouds with the galactic disk with a simple hydrodynamical code. Main aspects of the morphology of nearby (d 〈 500 pc) cloud complexes, like theρ Oph, Orion and Taurus-Auriga-Perseus complexes, are reproduced. These aspects include total mass, distance from the galactic plane, orientation of elongated gas structures with respect to the plane, and relative position of clusters of O-B stars with respect to the main concentrations of molecular gas. The space distribution of stars of different ages, usually explained in terms of sequential star formation, is interpreted in a new way in our model.
Type of Medium:
Electronic Resource
URL:
http://dx.doi.org/10.1007/BF00990054
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