N-Body models of M51: From extended tail to central spiral structure

Details N-Body models of M51: From extended tail to central spiral structure N-Body models of M51: From extended tail to central spiral structure

Jun 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001a%26at...20...93s&link_type=abstract

Astronomical and Astrophysical Transactions, vol. 20, Issue 1, pp.93-101

Astronomy and Astrophysics

Astronomy

Galaxy Dynamics, Galaxy Interactions, M51 (Ngc 5194/95)

Scientific paper

Various tidal models for M51 are reviewed, with the main emphasis on comparison with observed morphology and kinematics. Based on our current 3D self-gravitating simulations with up to 4 × 106 particles we propose that the 40° tilt of the extended HI tail, as well the high velocity material north of the companion are best explained in a model with a bound companion orbit. The same simulation models also suggest that the main spiral structure, including the inner spirals within 30", can be accounted for by a tidal perturbation propagating inward from the outer disc with the group velocity, as originally envisioned by Toomre (1969). During this evolution amplitude variations along the spiral arms arise, much as observed.

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