Dynamical Effects on Star Formation in Spiral Galaxies

Details Dynamical Effects on Star Formation in Spiral Galaxies Dynamical Effects on Star Formation in Spiral Galaxies

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aspc..275..315w&link_type=abstract

Disks of Galaxies: Kinematics, Dynamics and Peturbations, ASP Conference Proceedings, Vol. 275. Edited by E. Athanassoula, A. Bo

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Scientific paper

Most star formation in disk galaxies appears to occur spontaneously once molecular gas has formed. However, the star formation efficiency (SFE = SFR per unit H2 mass) is not always constant from one region of a galaxy to another. We show examples of galaxies where the SFE is reduced in regions where the kinematic signature of bar streaming is found. On the other hand, the SFE is enhanced in the inner Lindblad resonance ring of NGC 4736. Moreover, this ring exhibits a twofold symmetry in the distribution of HI and Hα emission but a threefold symmetry in the CO emission, indicating that the rate of massive star formation is dependent on location, not just the available gas mass. These results suggest that dynamics can play a role not just in organizing the gas, but also in triggering or inhibiting star formation.

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