Merging encounters between equal-mass non-rotating galaxies

Details Merging encounters between equal-mass non-rotating galaxies Merging encounters between equal-mass non-rotating galaxies

Jul 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989mnras.239..257n&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 239, July 15, 1989, p. 257-272. Research supported by C

Astronomy and Astrophysics

Astronomy

14

Galactic Mass, Galactic Rotation, Galactic Structure, Interacting Galaxies, Many Body Problem, Angular Momentum, Astronomical Models, Computerized Simulation, Gravitational Effects

Scientific paper

N-body simulations were performed in order to study merging encounters between equal-mass isotropic nonrotating de Vaucouleurs-type galaxies and to derive empirical correlations that relate the structural parameters of merger remnants to the initial orbit and structure of the progenitors. Galaxies which have experienced several mergers in the past are found to deviate systematically from the R(eff)-mu(eff) relation holding for normal elliptical galaxies, where R(eff) is the effective radius and mu(eff) is the logarithm of the surface density measured at the effective radius. The results suggest that some tidally distended galaxies may be interpreted as the remnants of mergers between galaxies of comparable mass and size.

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