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Testing hydrodynamics schemes in galaxy disc simulations
| Title: | Testing hydrodynamics schemes in galaxy disc simulations |
| Authors: | Few, C. G. Browse this author | | Dobbs, C. Browse this author | | Pettitt, A. Browse this author | | Konstandin, L. Browse this author |
| Issue Date: | May-2016 |
| Publisher: | Oxford University Press |
| Journal Title: | Monthly Notices of the Royal Astronomical Society |
| Volume: | 460 |
| Issue: | 4 |
| Start Page: | 4382 |
| End Page: | 4396 |
| Publisher DOI: | 10.1093/mnras/stw1226 |
| Abstract: | We examine how three fundamentally different numerical hydrodynamics codes follow the evolution of an isothermal galactic disc with an external spiral potential. We compare an adaptive mesh refinement code (RAMSES), a smoothed particle hydrodynamics code (SPHNG), and a volume-discretized mesh-less code (GIZMO). Using standard refinement criteria, we find that RAMSES produces a disc that is less vertically concentrated and does not reach such high densities as the SPHNG or GIZMO runs. The gas surface density in the spiral arms increases at a lower rate for the RAMSES simulations compared to the other codes. There is also a greater degree of substructure in the SPHNG and GIZMO runs and secondary spiral arms are more pronounced. By resolving the Jeans length with a greater number of grid cells, we achieve more similar results to the Lagrangian codes used in this study. Other alterations to the refinement scheme (adding extra levels of refinement and refining based on local density gradients) are less successful in reducing the disparity between RAMSES and SPHNG/GIZMO. Although more similar, SPHNG displays different density distributions and vertical mass profiles to all modes of GIZMO (including the smoothed particle hydrodynamics version). This suggests differences also arise which are not intrinsic to the particular method but rather due to its implementation. The discrepancies between codes (in particular, the densities reached in the spiral arms) could potentially result in differences in the locations and time-scales for gravitational collapse, and therefore impact star formation activity in more complex galaxy disc simulations. |
| Rights: | This article has been accepted for publication in Monthly notices of the royal astronomical society © 2016 The Authors Published by Oxford University Press on behalf of The Royal Astronomical Society. All rights reserved. |
| Type: | article |
| URI: | http://hdl.handle.net/2115/66598 |
| Appears in Collections: | 国際連携機構 (Institute for International Collaboration) > 雑誌発表論文等 (Peer-reviewed Journal Articles, etc)
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Submitter: PETTITT ALEXANDER ROBERT
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