Numerical Simulations of Major Barred Galaxies

Details Numerical Simulations of Major Barred Galaxies Numerical Simulations of Major Barred Galaxies

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...20921101y&link_type=abstract

2007 AAS/AAPT Joint Meeting, American Astronomical Society Meeting 209, #211.01; Bulletin of the American Astronomical Society,

Astronomy and Astrophysics

Astronomy

Scientific paper

Galaxies with major bars such as NGC1300 and NGC1097, are characterized by straight dust lanes, central starburst ring and outer spirals. Recent IR observations also show there are star formation patches and spur-like substructures. Through numerical simulations, we can reproduce the dust lanes, the central starburst ring, and the outer spirals by imposing a single strong bar potential on a self-gravitating gas disk. The strong bar potential also causes the disk to develop shear instability and Toomre’s instability in the case of self-gravitating disks, which lead to creation of the star formation patches and chaotic spur-like sub-structures. In our numerical simulations, we use the Antares code we develop, which adopts Cartesian coordinates and uses the high-order Godunov scheme with unsplit flux calculated from the exact Riemann solver. The self-gravitating forces are computed from the discreatization of Green’s kernel into the convolution formula and the fast Fourier transforms. This approach is different to the Fourier basis methods and our approach is the second order accuracy. The work is in parts supported by National Science Council, Taiwan, NSC95-2752-M-001-009-PAE.

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