Self-gravitating WARPS in disc galaxies

Details Self-gravitating WARPS in disc galaxies Self-gravitating WARPS in disc galaxies

Feb 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984mnras.206..691m&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 206, Feb. 1, 1984, p. 691-701.

Astronomy and Astrophysics

Astronomy

13

Disk Galaxies, Galactic Evolution, Galactic Structure, Computerized Simulation, Precession, Self Consistent Fields

Scientific paper

An N-body (particle-mesh) computer simulation is presented of the evolution of an initial warp in a self-gravitating disc galaxy. The initial warp has a tilted ring form, and the only external forces on the disc arise from a spherical halo component. The warp is found to retain ring symmetry at all times, and to behave dynamically rather like a system of concentric rigid rings. The qualitative evolution of the wrap is in good agreement with the predictions of Hunter & Toomre (1969) for a disc whose precession modes are barely discrete. Radial variations of precession rate combined with epicyclic phase-mixing mean that the warp gradually becomes smeared out. The difference in the evolution of self-gravitating and non-self-gravitating warps is emphasized.

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