Astronomy and Astrophysics – Astronomy
Scientific paper
May 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aas...180.4916g&link_type=abstract
American Astronomical Society, 180th AAS Meeting, #49.16; Bulletin of the American Astronomical Society, Vol. 24, p.811
Astronomy and Astrophysics
Astronomy
Scientific paper
We have obtained analytic expressions, in the impulse approximation, to describe the kinematic evolution of a stellar disk perturbed by the collision of a second galaxy perpendicular to, but not through the center of, the disk. For a certain range of parameters the disk responds first by forming a strong one-armed spiral feature when initially circular orbits deform and overlap. At later times a more axisymmetric ring-like structure develops if the collision occurs close enough to the disk center. The behavior of our model is verified with restricted three body simulations using assumptions similar to those of the analytic model. We then use a three-dimensional n-body/gas dynamics code to show similar behavior results from a collision between self-consistent, self-gravitating galaxies. The code employs a combination of particle-mesh and smoothed particle hydrodynamics techniques. Results obtained from this code show that high gas densities are reached in the same locations where the analytic model shows orbit crossing, that is, in a one-armed spiral feature. This is the location where we would predict active star formation to be taking place. At the same time, the stellar component of the galaxy forms two spiral-like arms. This likely arises from an instability in a disk that was only marginally stable before the collision. Gas density increases along these arms, but not to the extent found in the regions of orbit crossings.
Gerber Richard A.
Lamb Susan A.
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