Heating of galactic disks by mergers

Details Heating of galactic disks by mergers Heating of galactic disks by mergers

Jan 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...403...74q&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 403, no. 1, p. 74-93.

Statistics

Computation

305

Computational Astrophysics, Galactic Evolution, Galactic Structure, Interacting Galaxies, Spiral Galaxies, Abundance, Accretion Disks, Galactic Halos, Many Body Problem

Scientific paper

The paper considers dynamical aspects of mergers between disks and small satellite companions, with special attention given to: the self-consistent response of disks to satellite mergers, which generalizes an earlier investigation by Quinn & Goodman (1986); the evolution of satellite orbits and debris; and the long-term structure and kinematics of thickened disks as compared with observed properties of disk galaxies. For satellites with masses in the range 0.04-0.2 Mdisk on initially circular inclined prograde orbits merging with disks similar to the thin disk of the Galaxy, it is found that the dynamical coupling between disks and satellites leads to orbital decay. Disks respond to mergers by spreading both radially and vertically. The radial heating is driven largely by the spiral response of the dynamically cool disks to satellite perturbations.

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