Abstract
Dynamical evolution of galactic disks driven by interaction with satellite galaxies, particularly the problem of the disk warping and thickening is studied numerically. One of the main purpose of the study is to resolve the long standing problem of the origin of the disk warping. A possible cause of the warp is interaction with a satellite galaxy. In the case of the Milky Way, the LMC has been considered as the candidate. Some linear analysis have already given a positive result, but one had to wait for a fully self-consistent simulation as a proof. I have accomplished the numerical simulations with a million particles, by introducing a hybrid algorithm, SCF-TREE. Those simulations give us quantitative estimates for the Milky Way system. We have found an example in which large warp amplitudes are developed. We also found that the warp amplitudes depend on the halo distribution. Among our three models, the most massive and spherical halo is preferable for the observable warp excitation.
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References
Kuijken, K. and Dubinski, J.: 1995, Nearly self-consistent disc-bulge-halo models for galaxies, MNRAS 277, 1341.
Kuijken, K. and Gilmore, G.: 1991, The galactic disk surface mass density and the Galactic force K(z) at Z = 1.1 kiloparsecs, ApJL 367, L9.
Tsuchiya, T.: 2002, Contribution of the Large Magellanic Cloud to the Galactic warp, NewA 7(6), 293.
Vine, S. and Sigurdsson, S.: 1998, Simulations of spheroidal systems with substructure: trees in fields, MNRAS 295, 475.
Weinberg,M.D.: 1998, Dynamics of an interacting luminous disc, dark halo and satellite companion, MNRAS 299(2), 499.
Wilkinson, M.I. and Evans, N.W.: 1999, The present and future mass of the MilkyWay halo, MNRAS 310, 645.
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Tsuchiya, T. Dynamical evolution of galactic disks driven by interaction with a satellite. Astrophysics and Space Science 284, 515–518 (2003). https://doi.org/10.1023/A:1024016629743
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DOI: https://doi.org/10.1023/A:1024016629743