Models of star formation in interacting and merging disk galaxies

Details Models of star formation in interacting and merging disk galaxies Models of star formation in interacting and merging disk galaxies

Nov 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...400..153m&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 400, no. 1, p. 153-162.

Astronomy and Astrophysics

Astrophysics

96

Disk Galaxies, Interacting Galaxies, Star Formation Rate, Stellar Models, Interstellar Matter, Many Body Problem, Starburst Galaxies

Scientific paper

A series of models of interactions between star-forming disk galaxies is presented. The models employ an N-body code to calculate the gravitational dynamics, a discrete cloud model to govern the ISM dynamics, and a modified Schmidt law to describe star formation. Both merging galaxies and more distant flyby encounters, with differing disk orientations, are modeled. It is found that the global star formation rates (SFRs) in merging galaxies can be increased by an order of magnitude for several hundred million years, with the vast majority of the star formation arising in the central regions of the merging galaxies. Flyby encounters prove less successful at triggering starburst activity. To trigger any significant starburst, flybys must involve a relatively prograde disk; purely retrograde or highly inclined flybys have little effect on the global SFR of the participating disks. It is also found that the dissipative nature of the ISM can signficantly speed the merging process in some encounters.

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