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Theoretical Models of the Galactic Bulge

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Part of the book series: Astrophysics and Space Science Library ((ASSL,volume 418))

Abstract

Near infrared images from the COBE satellite presented the first clear evidence that our Milky Way galaxy contains a boxy shaped bulge. Recent years have witnessed a gradual paradigm shift in the formation and evolution of the Galactic bulge. Bulges were commonly believed to form in the dynamical violence of galaxy mergers. However, it has become increasingly clear that the main body of the Milky Way bulge is not a classical bulge made by previous major mergers, instead it appears to be a bar seen somewhat end-on. The Milky Way bar can form naturally from a precursor disc and thicken vertically by the internal firehose/buckling instability, giving rise to the boxy appearance. This picture is supported by many lines of evidence, including the asymmetric parallelogram shape, the strong cylindrical rotation (i.e., nearly constant rotation regardless of the height above the disc plane), the existence of an intriguing X-shaped structure in the bulge, and perhaps the metallicity gradients. We review the major theoretical models and techniques to understand the Milky Way bulge. Despite the progresses in recent theoretical attempts, a complete bulge formation model that explains the full kinematics and metallicity distribution is still not fully understood. Upcoming large surveys are expected to shed new light on the formation history of the Galactic bulge.

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Notes

  1. 1.

    It is puzzling why no galaxy has been caught in the process of violent buckling as shown in Fig. 10.2. The saturation timescale of the buckling instability is very rapid (about a few hundred Myr), but it is not short enough to miss out the violent buckling phase if one can observe thousands of edge-on barred galaxies. Perhaps this implies that the buckling instability must have happened in the very early assembly stage of disc galaxies, which is much harder to observe.

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Acknowledgements

We thank Shude Mao, Dimitri Gadotti, Eija Laurikainen, Zhi Li, Richard Long, Martin Smith, and Yu-jing Qin for helpful discussions and comments. The research presented here is partially supported by the 973 Program of China under grant no. 2014CB845700, by the National Natural Science Foundation of China under grant nos.11333003, 11322326, 11403072, and by the Strategic Priority Research Program “The Emergence of Cosmological Structures” (no. XDB09000000) of the Chinese Academy of Sciences. ZYL is grateful for the support from Shanghai Yangfan Talent Youth Program (No. 14YF1407700). This work made use of the facilities of the Center for High Performance Computing at Shanghai Astronomical Observatory.

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Correspondence to Juntai Shen .

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© 2016 Springer International Publishing Switzerland

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Shen, J., Li, ZY. (2016). Theoretical Models of the Galactic Bulge. In: Laurikainen, E., Peletier, R., Gadotti, D. (eds) Galactic Bulges. Astrophysics and Space Science Library, vol 418. Springer, Cham. https://doi.org/10.1007/978-3-319-19378-6_10

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