Comparing simulations of AGN feedback
We perform adaptive mesh refinement (AMR) and smoothed particle hydrodynamics (SPH) cosmological zoom simulations of a region around a forming galaxy cluster, comparing the ability of the methods to handle successively more complex baryonic physics. In the simplest, non-radiative case, the two metho...
| Հիմնական հեղինակներ: | , , , , , , , |
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| Ձևաչափ: | Journal article |
| Հրապարակվել է: |
American Astronomical Society
2016
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| _version_ | 1826291919830908928 |
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| author | Richardson, M Scannapieco, E Devriendt, J Slyz, A Thacker, R Dubois, Y Wurster, J Silk, J |
| author_facet | Richardson, M Scannapieco, E Devriendt, J Slyz, A Thacker, R Dubois, Y Wurster, J Silk, J |
| author_sort | Richardson, M |
| collection | OXFORD |
| description | We perform adaptive mesh refinement (AMR) and smoothed particle hydrodynamics (SPH) cosmological zoom simulations of a region around a forming galaxy cluster, comparing the ability of the methods to handle successively more complex baryonic physics. In the simplest, non-radiative case, the two methods are in good agreement with each other, but the SPH simulations generate central cores with slightly lower entropies and virial shocks at slightly larger radii, consistent with what has been seen in previous studies. The inclusion of radiative cooling, star formation, and stellar feedback leads to much larger differences between the two methods. Most dramatically, at z=5, rapid cooling in the AMR case moves the accretion shock well within the virial radius, while this shock remains near the virial radius in the SPH case, due to excess heating, coupled with poorer capturing of the shock width. On the other hand, the addition of feedback from active galactic nuclei (AGN) to the simulations results in much better agreement between the methods. In this case both simulations display halo gas entropies of 100 keV cm^2, similar decrements in the star-formation rate, and a drop in the halo baryon content of roughly 30%. This is consistent with AGN growth being self-regulated, regardless of the numerical method. However, the simulations with AGN feedback continue to differ in aspects that are not self-regulated, such that in SPH a larger volume of gas is impacted by feedback, and the cluster still has a lower entropy central core. |
| first_indexed | 2024-03-07T03:06:44Z |
| format | Journal article |
| id | oxford-uuid:b2ccf4df-56c7-4232-a413-9093944ee1ae |
| institution | University of Oxford |
| last_indexed | 2024-03-07T03:06:44Z |
| publishDate | 2016 |
| publisher | American Astronomical Society |
| record_format | dspace |
| spelling | oxford-uuid:b2ccf4df-56c7-4232-a413-9093944ee1ae2022-03-27T04:14:18ZComparing simulations of AGN feedbackJournal articlehttp://purl.org/coar/resource_type/c_dcae04bcuuid:b2ccf4df-56c7-4232-a413-9093944ee1aeSymplectic Elements at OxfordAmerican Astronomical Society2016Richardson, MScannapieco, EDevriendt, JSlyz, AThacker, RDubois, YWurster, JSilk, JWe perform adaptive mesh refinement (AMR) and smoothed particle hydrodynamics (SPH) cosmological zoom simulations of a region around a forming galaxy cluster, comparing the ability of the methods to handle successively more complex baryonic physics. In the simplest, non-radiative case, the two methods are in good agreement with each other, but the SPH simulations generate central cores with slightly lower entropies and virial shocks at slightly larger radii, consistent with what has been seen in previous studies. The inclusion of radiative cooling, star formation, and stellar feedback leads to much larger differences between the two methods. Most dramatically, at z=5, rapid cooling in the AMR case moves the accretion shock well within the virial radius, while this shock remains near the virial radius in the SPH case, due to excess heating, coupled with poorer capturing of the shock width. On the other hand, the addition of feedback from active galactic nuclei (AGN) to the simulations results in much better agreement between the methods. In this case both simulations display halo gas entropies of 100 keV cm^2, similar decrements in the star-formation rate, and a drop in the halo baryon content of roughly 30%. This is consistent with AGN growth being self-regulated, regardless of the numerical method. However, the simulations with AGN feedback continue to differ in aspects that are not self-regulated, such that in SPH a larger volume of gas is impacted by feedback, and the cluster still has a lower entropy central core. |
| spellingShingle | Richardson, M Scannapieco, E Devriendt, J Slyz, A Thacker, R Dubois, Y Wurster, J Silk, J Comparing simulations of AGN feedback |
| title | Comparing simulations of AGN feedback |
| title_full | Comparing simulations of AGN feedback |
| title_fullStr | Comparing simulations of AGN feedback |
| title_full_unstemmed | Comparing simulations of AGN feedback |
| title_short | Comparing simulations of AGN feedback |
| title_sort | comparing simulations of agn feedback |
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