Abstract
Boxy/peanut-shaped bulge galaxies constitute at least 20–30% of all spirals. Distribution functions and numerical simulations studies have shown that the slow decay of the orbit of a companion into a larger spiral can lead to the formation of a boxy/peanut bulge. However, the bar-buckling instability now appears a more likely process. Thin bars either do not form or, as shown by N-body simulations, buckle and settle with an increased thickness, appearing boxy or peanut-shaped when seen edge-on. This project aims to determine the dynamical state of a sample of 30 edge-on spirals, 3/4 of which have boxy/peanut-shaped bulges, half having close-by companions.
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© 1999 Springer Science+Business Media Dordrecht
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Bureau, M., Freeman, K.C. (1999). Formation of Boxy/Peanut-Shaped Bulges in Spiral Galaxies: Accretion or Bar Instability?. In: Barnes, J.E., Sanders, D.B. (eds) Galaxy Interactions at Low and High Redshift. International Astronomical Union, vol 186. Springer, Dordrecht. https://doi.org/10.1007/978-94-011-4665-4_41
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DOI: https://doi.org/10.1007/978-94-011-4665-4_41
Publisher Name: Springer, Dordrecht
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