Simulations of the grand design galaxy M51: a case study for analysing tidally induced spiral structure

By C. Dobbs, Ch. Theis, J. E. Pringle, Matthew R. Bate. 2009

145 citations recorded by the source corpus.

We present hydrodynamical models of the grand design spiral M51 (NGC 5194), and its interaction with its companion NGC 5195. Despite the simplicity of our models, our simulations capture the present day spiral structure of M51 remarkably well, and even reproduce details such as a kink along one spiral arm, and spiral arm bifurcations. We investigate the oset between the stellar and gaseous spiral arms, and nd at most times (including the present day) there is no oset between the stars and gas to within our error bars. We also compare our simulations with recent observational analysis of M51. We compute the pattern speed versus radius, and like the observations, nd no single global pattern speed. We also show that the spiral arms cannot be tted well by logarithmic spirals. We interpret these ndings as evidence that M51 does not exhibit a quasi-steady density wave, as would be predicted by density wave theory. The internal structure of M51 derives from the complicated and dynamical interaction with its companion, resulting in spiral arms showing considerable structure in the form of short-lived kinks and bifurcations. Rather than trying to model such galaxies in terms of global spiral modes with

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/45f2c32d8df58f1ebfc869c299b0830acc5b6ff1

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In Astronomy and Astrophysics

1. J. Baba
2. C. Dobbs
3. R. Grand
4. M. Cropper
5. Daisuke Kawata
6. J. Sellwood
7. I. Minchev
8. James Wadsley

Citations in the corpus

• Dawes Review 4: Spiral Structures in Disc Galaxies (2014, background): “For M51, the best matched orbit of M51 and NGC5195 currently involves two orbits of the NGC 5195 around M51, after which the two galaxies merge (Salo & Laurikainen 2000a; Theis & Spinneker 2003).”
• The dynamics of stars around spiral arms (2011, background): “Numerical simulations of an interacting galaxy in Dobbs et al. (2010) also shows a pattern speed that decreases as a function of radius.”
• The lifetimes of spiral patterns in disc galaxies (2010, background): “There seems little doubt that a tidally-driven spiral pattern evolves rapidly (e.g. Salo & Laurikainen 1993; Dobbs et al. 2010), but repeated excitations may be possible (Byrd & Howard 1992).”