Physics
Scientific paper
May 1995
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995a%26a...297...37c&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 297, no. 1, p. 37-48
Physics
34
Elliptical Galaxies, Galactic Rotation, Interacting Galaxies, Stellar Motions, Stellar Physics, Velocity Distribution, Astronomical Models, Computerized Simulation, Galactic Structure, Perturbation, Radii, Two Body Problem
Scientific paper
We have presented in a companion article a kinematic study of three E+E galaxy pairs, NGC741/742, 1587/1588 (CPG 99) and 2672/2673 (CPG 175). We find some evidence for perturbed velocity dispersion profiles. These perturbation features are now reported for 14 galaxies in the literature. They occur, or require observations for detection, at large radii where the S/N in the data is low. While observations of individual galaxies are sometimes uncertain, the large number of objects where such features are suspected gives confidence that they are real. These perturbations can be attributed to projection effects contamination along the line of sight, or directly to the tidal interaction. We report the results of several self-gravitating simulations of unbound pairs in an effort to better understand these perturbations another generic features of close E+E pairs reported in the literature. The models frequently show off-center envelopes created by the asymmetry of tidal forces during interpenetrating encounters. The envelopes last for a few 108 yrs, which explains the frequency of such features in observed pairs. This phenomenon is stronger in the self-gravitating simulations than in the MTBA runs. U-shaped (and an equal number of inverse U shaped velocity profiles are seen in the simulations, a result of ablation in the outer envelopes. Simulations including inner galaxy rotation also preserve this feature, irrespective of the spin vector direction in each galaxy. U-shape velocity structure is found to be a robust indicator of the ongoing interaction. All simulations show evidence for enhanced velocity dispersion between the galaxies even in the case of simple superposition of two non interacting objects. We therefore conclude that this cannot be considered an unambiguous indicator of the interaction.
Bonfanti P. P.
Combes François
Prugniel Philippe
Rampazzo Roberto
Sulentic Jack W.
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