Simulations of merging disk galaxies

Details Simulations of merging disk galaxies Simulations of merging disk galaxies

Aug 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982apj...259..103f&link_type=abstract

Astrophysical Journal, Part 1, vol. 259, Aug. 1, 1982, p. 103-115.

Mathematics

Logic

79

Astronomical Models, Disk Galaxies, Galactic Evolution, Galactic Structure, Elliptical Galaxies, Galactic Rotation, Luminosity, Many Body Problem, Simulation

Scientific paper

A systematic study is attempted of the conditions under which two identical disk-halo galaxies can be expected to merge, and of the observational properties of the resulting merger remnants. The galaxy models employed are described and their intrinsic stability assessed. A reliable criterion for the merging of these systems is formulated for the particular case when both spins are aligned with the orbital angular momentum. The effect on merging of varying the relative disk orientations for a single parabolic encounter is studied. It is found that the merging of disk galaxies can lead to objects remarkably similar to elliptical galaxies in terms of morphology, luminosity profile, core radius, central velocity dispersion, rotation curves, and metallicity gradients. Both the present apparent rate of galaxy merging and the numbers predicted by cosmological merging simulations suggest that the Universe contains many merger remnants.

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