Kinematic structures of merger remnants

Details Kinematic structures of merger remnants Kinematic structures of merger remnants

Dec 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991pasj...43..781o&link_type=abstract

Astronomical Society of Japan, Publications (ISSN 0004-6264), vol. 43, no. 6, 1991, p. 781-793.

Astronomy and Astrophysics

Astronomy

16

Disk Galaxies, Elliptical Galaxies, Interacting Galaxies, Kinematics, Many Body Problem, Computerized Simulation, Extremely High Frequencies, Star Formation

Scientific paper

A set of N-body simulations of the merging of two identical spherical galaxies using a special-purpose computer, GRAPE-1 are performed. It is found that the kinematic properties of the resulting merger remnants are consistent with those of observed elliptical galaxies. The ratios of the maximum rotation velocity (Vmax) to the velocity dispersion (sigma0) are smaller than 0.6, even in the case of large impact parameters. This is in good agreement with the lack of elliptical galaxies whose (Vmax)/sigma0 exceeds 0.6. Previous N-body calculations have contradicted the observed kinematic studies of elliptical galaxies, because relaxation was numerically enhanced due to the small number of particles (about 500). Simulations with N = 16384 resolve this problem. The central velocity dispersion increased by 10-20 percent through merging for a wide range of impact parameters. This increase is consistent with the Faber-Jackson relation.

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