Other
Scientific paper
Aug 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...431..604g&link_type=abstract
The Astrophysical Journal, vol. 431, no. 2, pt. 1, p. 604-616
Other
19
Collision Parameters, Disk Galaxies, Galactic Evolution, Interacting Galaxies, Mathematical Models, Spiral Galaxies, Star Formation, Stellar Rotation, Computerized Simulation, Cosmology, Gas Dynamics, Kinematics, Many Body Problem, Perturbation Theory, Stellar Orbits, Stellar Oscillations
Scientific paper
We derive analytic expressions, using the impulse and epicycle approximations, which describe the kinematic response of a disk galaxy following a collision with a second spherical galaxy which collides perpendicular to, but not through the center of, the disk. This model can reporduce the morphologies found in n-body experiments in which distant encounters produce two-armed spiral patterns and more central collisions produce rings in the disk galaxy, thereby confirming that simple kinematics can be used to describe the early evolution of these systems. Application of this procedure provides a convenient method with which to conduct parameter studies of these collisions. Comparison of the kinematic description with a fully self-gravitating, three-dimensional n-body/gasdynamics computer model shows that the disk galaxy's response is initially well represented by the kinematic model but that the self-gravity of the disk becomes important at longer times after the collision. The flows of gas and stars decouple from one another where stellar orbits cross, leaving regions of elevated gas density behind as the stars move freely past each other. If star formation rates are enhanced in these regions of high gas density, active star formation could be taking place where there is no corresponding dense feature in the old stellar population.
Gerber Richard A.
Lamb Susan A.
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