Spiral modes driven by narrow features in angular-momentum density

Details Spiral modes driven by narrow features in angular-momentum density Spiral modes driven by narrow features in angular-momentum density

May 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991mnras.250..278s&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 250, May 15, 1991, p. 278-299.

Astronomy and Astrophysics

Astronomy

74

Angular Momentum, Density Distribution, Disk Galaxies, Astronomical Models, Computerized Simulation, Equations Of Motion, Gravitational Fields

Scientific paper

Computer simulations are used to demonstrate that a galaxy disk is destabilized by many types of narrow axisymmetric feature in the angular-momentum density distribution of particles. The vigorously growing disturbances, which can develop even in disks having considerable random motion, have a large-scale spiral form. The instabilities associated with a narrow groove are of particular interest, but narrow ridges and features having more complicated profiles are also destabilizing. An approximate local analysis is presented which reveals the mechanism for the modes and predicts frequencies for both groove and ridge modes in rough agreement with those from the global simulations.

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