Global-, local-, and intermediate-scale structures in prototype spiral galaxies

Details Global-, local-, and intermediate-scale structures in prototype spiral galaxies Global-, local-, and intermediate-scale structures in prototype spiral galaxies

Jun 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993pasp..105..670r&link_type=abstract

Astronomical Society of the Pacific, Publications (ISSN 0004-6280), vol. 105, no. 688, p. 670-673.

Statistics

Computation

10

Galactic Structure, Spiral Galaxies, Gas Dynamics, Shock Waves, Supernovae

Scientific paper

The relationship between galactic spiral structure and the matter in the underlying disk constitutes one of the central problems in galactic dynamics. In Bertin et al. (1989), disk matter characterized by a low-dispersive speed is shown to be capable of playing a key role in the generation of large-scale spiral structure. In Roberts et al. (1992), this self-gravitating, low-dispersion disk matter is shown to be capable of playing an essential role in the formation of structure on local and intermediate scales. Both in computed cases where large-scale spiral structure is present and in those where it is not, the same dominant physical processes and fundamental dynamical mechanisms are active on local scales. The new perception, in which large-scale and small-scale phenomena operate somewhat independently as evidenced in the computational studies, permits a range of flocculent, multiarmed, and grand design spiral types to be simulated. In particular, grand design galaxies with ragged appearances exhibiting spurs, arm branchings, and interarm bridges in addition to the major spiral arms, similar to those often observed, can be generated.

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