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C. Yuan (ASIAA, Taipei, Taiwan, ROC), D.C.C. Yen (ASIAA and Pu-Jen University, Taipei, Taiwan, ROC)
In this report, we will show the results of our numerical simulations of a self-gravitating disk subject to a rotating bar force. Normally, spiral density waves are excited at three resonances in the disk, namely, the outer Lindblad resonance (OLR), the outer inner Lindblad resonance (OILR), and the inner inner Lindblad resonances (IILR). Associated with these waves are the angular momentum transports between the disk and the bar, and gas in the disk will redistribute accordingly. Gas accumulated near the OLR often becomes unstable and develops into chaos. Waves at different resonances can interact to form spiral-ring patterns. We will present the following simulations: (1) disk with the presence of all three resonances. (2) interaction between leading spirals excited at IILR and trailing spirals at OILR, (3) the chaotic pattern at OLR and the stable disk with high surface density near the center (OILR), and (4) simulation of waves driven a major bar, such as NGC5248. We use the high-order Godunov codes we developed, with FFT Poisson solver. The work is supported in parts by a Key Project of Academia Sinica and National Science Council grant 91-2112-M-011-070.
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Bulletin of the American Astronomical Society, 35#5
© 2003. The American Astronomical Soceity.