Time evolution of galactic warps in prolate haloes |
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| Authors: | M Ideta S Hozumi T Tsuchiya M Takizawa |
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| Institution: | Department of Astronomy, Faculty of Science, Kyoto University, Kyoto 606-8502, Japan; Faculty of Education, Shiga University, 2-5-1 Hiratsu, Otsu, Shiga 520-0862, Japan; Department of Earth and Space Science, Graduate School of Science, Osaka University, Machikaneyama‐cho, Toyonaka 560‐0043, Japan; Research Center for the Early Universe, Graduate School of Science, University of Tokyo, Bunkyo‐ku, Tokyo 113‐0033, Japan |
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| Abstract: | A recent observation with the Hipparcos satellite and some numerical simulations imply that the interaction between an oblate halo and a disc is inappropriate for the persistence of galactic warps. Following on from this , we have compared the time evolution of galactic warps in a prolate halo with that in an oblate halo. The haloes were approximated as fixed potentials, while the discs were represented by N -body particles. We have found that the warping in the oblate halo continues to wind up, and finally disappears. On the other hand, for the prolate halo model, the precession rate of the outer disc increases when the precession of the outer disc recedes from that of the inner disc, and vice versa. Consequently, the warping in the prolate halo persisted to the end of the simulation by retaining the alignment of the line of nodes of the warped disc. Therefore, our results suggest that prolate haloes could sustain galactic warps. The physical mechanism of the persistence of warp is discussed on the basis of the torque between a halo and a disc and that between the inner and outer regions of the disc. |
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| Keywords: | methods: numerical galaxies: haloes galaxies: kinematics and dynamics galaxies: structure |
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