Shock finding on a moving-mesh – II. Hydrodynamic shocks in the Illustris universe
Hydrodynamical shocks are a manifestation of the non-linearity of the Euler equations and play a fundamental role in cosmological gas dynamics. In this work, we identify and analyse shocks in the Illustris simulation, and contrast the results with those of non-radiative runs. We show that simulation...
| Main Authors: | , , , , , , , , , |
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| Format: | Article |
| Language: | en_US |
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Oxford University Press
2017
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| Online Access: | http://hdl.handle.net/1721.1/108546 https://orcid.org/0000-0001-8593-7692 |
| _version_ | 1811080961219100672 |
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| author | Schaal, Kevin Springel, Volker Pakmor, Rüdiger Pfrommer, Christoph Nelson, Dylan Vogelsberger, Mark Genel, Shy Pillepich, Annalisa Sijacki, Debora Hernquist, Lars |
| author2 | Massachusetts Institute of Technology. Department of Physics |
| author_facet | Massachusetts Institute of Technology. Department of Physics Schaal, Kevin Springel, Volker Pakmor, Rüdiger Pfrommer, Christoph Nelson, Dylan Vogelsberger, Mark Genel, Shy Pillepich, Annalisa Sijacki, Debora Hernquist, Lars |
| author_sort | Schaal, Kevin |
| collection | MIT |
| description | Hydrodynamical shocks are a manifestation of the non-linearity of the Euler equations and play a fundamental role in cosmological gas dynamics. In this work, we identify and analyse shocks in the Illustris simulation, and contrast the results with those of non-radiative runs. We show that simulations with more comprehensive physical models of galaxy formation pose new challenges for shock finding algorithms due to radiative cooling and star-forming processes, prompting us to develop a number of methodology improvements. We find in Illustris a total shock surface area which is about 1.4 times larger at the present epoch compared to non-radiative runs, and an energy dissipation rate at shocks which is higher by a factor of around 7. Remarkably, shocks with Mach numbers above and below
M≈10
contribute about equally to the total dissipation across cosmic time. This is in sharp contrast to non-radiative simulations, and we demonstrate that a large part of the difference arises due to strong black hole radio-mode feedback in Illustris. We also provide an overview of the large diversity of shock morphologies, which includes complex networks of halo-internal shocks, shocks on to cosmic sheets, feedback shocks due to black holes and galactic winds, as well as ubiquitous accretion shocks. In high-redshift systems more massive than 10¹² M⊙, we discover the existence of a double accretion shock pattern in haloes. They are created when gas streams along filaments without being shocked at the outer accretion shock, but then forms a second, roughly spherical accretion shock further inside. |
| first_indexed | 2024-09-23T11:39:35Z |
| format | Article |
| id | mit-1721.1/108546 |
| institution | Massachusetts Institute of Technology |
| language | en_US |
| last_indexed | 2024-09-23T11:39:35Z |
| publishDate | 2017 |
| publisher | Oxford University Press |
| record_format | dspace |
| spelling | mit-1721.1/1085462022-10-01T05:06:31Z Shock finding on a moving-mesh – II. Hydrodynamic shocks in the Illustris universe Schaal, Kevin Springel, Volker Pakmor, Rüdiger Pfrommer, Christoph Nelson, Dylan Vogelsberger, Mark Genel, Shy Pillepich, Annalisa Sijacki, Debora Hernquist, Lars Massachusetts Institute of Technology. Department of Physics MIT Kavli Institute for Astrophysics and Space Research Vogelsberger, Mark Hydrodynamical shocks are a manifestation of the non-linearity of the Euler equations and play a fundamental role in cosmological gas dynamics. In this work, we identify and analyse shocks in the Illustris simulation, and contrast the results with those of non-radiative runs. We show that simulations with more comprehensive physical models of galaxy formation pose new challenges for shock finding algorithms due to radiative cooling and star-forming processes, prompting us to develop a number of methodology improvements. We find in Illustris a total shock surface area which is about 1.4 times larger at the present epoch compared to non-radiative runs, and an energy dissipation rate at shocks which is higher by a factor of around 7. Remarkably, shocks with Mach numbers above and below M≈10 contribute about equally to the total dissipation across cosmic time. This is in sharp contrast to non-radiative simulations, and we demonstrate that a large part of the difference arises due to strong black hole radio-mode feedback in Illustris. We also provide an overview of the large diversity of shock morphologies, which includes complex networks of halo-internal shocks, shocks on to cosmic sheets, feedback shocks due to black holes and galactic winds, as well as ubiquitous accretion shocks. In high-redshift systems more massive than 10¹² M⊙, we discover the existence of a double accretion shock pattern in haloes. They are created when gas streams along filaments without being shocked at the outer accretion shock, but then forms a second, roughly spherical accretion shock further inside. 2017-05-01T18:20:03Z 2017-05-01T18:20:03Z 2016-07 2016-06 Article http://purl.org/eprint/type/JournalArticle 0035-8711 1365-2966 http://hdl.handle.net/1721.1/108546 Schaal, Kevin; Springel, Volker; Pakmor, Rüdiger; Pfrommer, Christoph; Nelson, Dylan; Vogelsberger, Mark; Genel, Shy; Pillepich, Annalisa; Sijacki, Debora and Hernquist, Lars. “Shock Finding on a Moving-Mesh – II. Hydrodynamic Shocks in the Illustris Universe.” Monthly Notices of the Royal Astronomical Society 461, no. 4 (July 2016): 4441–4465. https://orcid.org/0000-0001-8593-7692 en_US http://dx.doi.org/10.1093/mnras/stw1587 Monthly Notices of the Royal Astronomical Society Creative Commons Attribution-Noncommercial-Share Alike http://creativecommons.org/licenses/by-nc-sa/4.0/ application/pdf Oxford University Press arXiv |
| spellingShingle | Schaal, Kevin Springel, Volker Pakmor, Rüdiger Pfrommer, Christoph Nelson, Dylan Vogelsberger, Mark Genel, Shy Pillepich, Annalisa Sijacki, Debora Hernquist, Lars Shock finding on a moving-mesh – II. Hydrodynamic shocks in the Illustris universe |
| title | Shock finding on a moving-mesh – II. Hydrodynamic shocks in the Illustris universe |
| title_full | Shock finding on a moving-mesh – II. Hydrodynamic shocks in the Illustris universe |
| title_fullStr | Shock finding on a moving-mesh – II. Hydrodynamic shocks in the Illustris universe |
| title_full_unstemmed | Shock finding on a moving-mesh – II. Hydrodynamic shocks in the Illustris universe |
| title_short | Shock finding on a moving-mesh – II. Hydrodynamic shocks in the Illustris universe |
| title_sort | shock finding on a moving mesh ii hydrodynamic shocks in the illustris universe |
| url | http://hdl.handle.net/1721.1/108546 https://orcid.org/0000-0001-8593-7692 |
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