Spiral structure and star formation. II - Stellar lifetimes and cloud kinematics

Details Spiral structure and star formation. II - Stellar lifetimes and cloud kinematics Spiral structure and star formation. II - Stellar lifetimes and cloud kinematics

Jul 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984apj...282..106h&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 282, July 1, 1984, p. 106-117.

Other

56

Interstellar Matter, Molecular Clouds, Spiral Galaxies, Star Formation, Density Distribution, Density Wave Model, Galactic Structure, Gas Dynamics, Mean Free Path, Velocity Distribution

Scientific paper

The reliability studies using continuum gas dynamical calculations becomes questionable in connection with the apparent clumpiness of the Galaxy's interstellar medium (ISM). Roberts and Hausman (1984) have, therefore, presented a detailed model of a disk galaxy in which the ISM consists entirely of 'cloud particles', which orbit ballistically in the galaxy's gravitational field, collide inelastically with one another, and give birth to and subsequently interact with young star associations. The effects of changing the clouds's collisional mean free path have been examined, and the variations in the young star system's spiral morphology have been explored. The present investigation is concerned with a further study of this clumpy, cloudy ISM model, taking into account longer mean free path models likely to be appropriate for systems of molecular clouds. Attention is also given to the kinematics of clouds as they orbit under the influence of galactic gravity, collisions, and supernova remnants.

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