Astronomy and Astrophysics – Astrophysics
Scientific paper
Apr 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aps..aprb17104m&link_type=abstract
American Physical Society, April Meeting, Jointly Sponsored with the High Energy Astrophysics Division (HEAD) of the American As
Astronomy and Astrophysics
Astrophysics
Scientific paper
We present a survey of numerical simulations of colliding disk galaxies in which a significant component of the impact velocity is parallel to the spin axes of the galaxies. The effects of varying the impact velocity, the distance between the disk centers at impact, and the relative orientation of the disks are explored. The simulations employ an N-body treatment of the stars and dark matter, together with a Smooth Particle Hydrodynamics treatment of the gas, in which all six components of the models (two dark halos, gaseous disks, and stellar disks) are gravitationally active. The results indicate that for such impact geometries, collisions of co-rotating gaseous disks can lead to the very rapid formation of a central, dense gas disk, and that in all cases extensive star formation is predicted by the very high gas densities obtained. Simultaneously, gas and stars are dispersed over very large volumes. A video demonstrating some of these results will be presented. We would like to acknowledge support from DOE B506657.
Hearn Nathan C.
Kwon Soojin
Lamb Susan A.
Morgan John P.
No associations
LandOfFree
Simulations of Collisions and Merging of Disk Galaxies using N-body/SPH computations does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Simulations of Collisions and Merging of Disk Galaxies using N-body/SPH computations, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Simulations of Collisions and Merging of Disk Galaxies using N-body/SPH computations will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1535795