The XMAGNET Exascale MHD Simulations of SMBH Feedback in Galaxy Groups and Clusters: Overview and Preliminary Cluster Results
We present initial results from extremely well-resolved 3D magnetohydrodynamical simulations of idealized galaxy clusters, conducted using the AthenaPK code on the Frontier exascale supercomputer. These simulations explore the self-regulation of galaxy groups and cool-core clusters by cold gas-trigg...
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2025-01-01
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| Series: | The Astrophysical Journal |
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| Online Access: | https://doi.org/10.3847/1538-4357/adde45 |
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| author | Philipp Grete Brian W. O’Shea Forrest W. Glines Deovrat Prasad Benjamin D. Wibking Martin Fournier Marcus Brüggen G. Mark Voit |
| author_facet | Philipp Grete Brian W. O’Shea Forrest W. Glines Deovrat Prasad Benjamin D. Wibking Martin Fournier Marcus Brüggen G. Mark Voit |
| author_sort | Philipp Grete |
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| description | We present initial results from extremely well-resolved 3D magnetohydrodynamical simulations of idealized galaxy clusters, conducted using the AthenaPK code on the Frontier exascale supercomputer. These simulations explore the self-regulation of galaxy groups and cool-core clusters by cold gas-triggered active galactic nucleus (AGN) feedback incorporating magnetized kinetic jets. Our simulation campaign includes simulations of galaxy groups and clusters with a range of masses and intragroup and intracluster medium properties. In this paper, we present results that focus on a Perseus-like cluster. We find that the simulated clusters are self-regulating, with the cluster cores staying at a roughly constant thermodynamic state and AGN jet power staying at physically reasonable values (≃10 ^44 –10 ^45 erg s ^–1 ) for billions of years without a discernible duty cycle. These simulations also produce significant amounts of cold gas, with calculations having strong magnetic fields generally both promoting cold gas formation and allowing cold gas out to much larger cluster-centric radii (≃100 kpc) than simulations with weak or no fields (≃10 kpc), and also having more filamentary cold gas morphology. We find that AGN feedback significantly increases the strength of magnetic fields at the center of the cluster. We also find that the magnetized turbulence generated by the AGN results in turbulence where the velocity power spectra are tied to AGN activity, whereas the magnetic energy spectra are much less impacted after reaching a stationary state. |
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| institution | Kabale University |
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| language | English |
| publishDate | 2025-01-01 |
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| spelling | doaj-art-3365e240ee0c40cf80c3cff32c1af2032025-08-20T03:51:29ZengIOP PublishingThe Astrophysical Journal1538-43572025-01-01988215510.3847/1538-4357/adde45The XMAGNET Exascale MHD Simulations of SMBH Feedback in Galaxy Groups and Clusters: Overview and Preliminary Cluster ResultsPhilipp Grete0https://orcid.org/0000-0003-3555-9886Brian W. O’Shea1https://orcid.org/0000-0002-2786-0348Forrest W. Glines2https://orcid.org/0000-0002-6837-8195Deovrat Prasad3https://orcid.org/0000-0003-1255-6375Benjamin D. Wibking4https://orcid.org/0000-0003-3175-2291Martin Fournier5https://orcid.org/0009-0006-2593-1583Marcus Brüggen6https://orcid.org/0000-0002-3369-7735G. Mark Voit7https://orcid.org/0000-0002-3514-0383University of Hamburg , Hamburger Sternwarte, Gojenbergsweg 112, 21029 Hamburg, GermanyDepartment of Computational Mathematics, Science, & Engineering, Michigan State University , 428 S. Shaw Lane, East Lansing, MI 48824, USA; Department of Physics & Astronomy, 567 Wilson Road, Michigan State University , East Lansing, MI 48824, USA; Facility for Rare Isotope Beams, Michigan State University , 640 S. Shaw Lane, East Lansing, MI 48824, USA; Institute for Cyber-Enabled Research, 567 Wilson Road, Michigan State University , East Lansing, MI 48824, USATheoretical Division , TA-3 Bldg. 123, Los Alamos National Laboratory, Los Alamos, NM 87545, USASchool of Physics and Astronomy, Cardiff University , 5 The Parade, Cardiff CF24 3AA, UKDepartment of Physics & Astronomy, 567 Wilson Road, Michigan State University , East Lansing, MI 48824, USAUniversity of Hamburg , Hamburger Sternwarte, Gojenbergsweg 112, 21029 Hamburg, GermanyUniversity of Hamburg , Hamburger Sternwarte, Gojenbergsweg 112, 21029 Hamburg, GermanyDepartment of Physics & Astronomy, 567 Wilson Road, Michigan State University , East Lansing, MI 48824, USAWe present initial results from extremely well-resolved 3D magnetohydrodynamical simulations of idealized galaxy clusters, conducted using the AthenaPK code on the Frontier exascale supercomputer. These simulations explore the self-regulation of galaxy groups and cool-core clusters by cold gas-triggered active galactic nucleus (AGN) feedback incorporating magnetized kinetic jets. Our simulation campaign includes simulations of galaxy groups and clusters with a range of masses and intragroup and intracluster medium properties. In this paper, we present results that focus on a Perseus-like cluster. We find that the simulated clusters are self-regulating, with the cluster cores staying at a roughly constant thermodynamic state and AGN jet power staying at physically reasonable values (≃10 ^44 –10 ^45 erg s ^–1 ) for billions of years without a discernible duty cycle. These simulations also produce significant amounts of cold gas, with calculations having strong magnetic fields generally both promoting cold gas formation and allowing cold gas out to much larger cluster-centric radii (≃100 kpc) than simulations with weak or no fields (≃10 kpc), and also having more filamentary cold gas morphology. We find that AGN feedback significantly increases the strength of magnetic fields at the center of the cluster. We also find that the magnetized turbulence generated by the AGN results in turbulence where the velocity power spectra are tied to AGN activity, whereas the magnetic energy spectra are much less impacted after reaching a stationary state.https://doi.org/10.3847/1538-4357/adde45Galaxy clustersGalaxy jetsIntracluster mediumMagnetic fieldsMagnetohydrodynamical simulations |
| spellingShingle | Philipp Grete Brian W. O’Shea Forrest W. Glines Deovrat Prasad Benjamin D. Wibking Martin Fournier Marcus Brüggen G. Mark Voit The XMAGNET Exascale MHD Simulations of SMBH Feedback in Galaxy Groups and Clusters: Overview and Preliminary Cluster Results The Astrophysical Journal Galaxy clusters Galaxy jets Intracluster medium Magnetic fields Magnetohydrodynamical simulations |
| title | The XMAGNET Exascale MHD Simulations of SMBH Feedback in Galaxy Groups and Clusters: Overview and Preliminary Cluster Results |
| title_full | The XMAGNET Exascale MHD Simulations of SMBH Feedback in Galaxy Groups and Clusters: Overview and Preliminary Cluster Results |
| title_fullStr | The XMAGNET Exascale MHD Simulations of SMBH Feedback in Galaxy Groups and Clusters: Overview and Preliminary Cluster Results |
| title_full_unstemmed | The XMAGNET Exascale MHD Simulations of SMBH Feedback in Galaxy Groups and Clusters: Overview and Preliminary Cluster Results |
| title_short | The XMAGNET Exascale MHD Simulations of SMBH Feedback in Galaxy Groups and Clusters: Overview and Preliminary Cluster Results |
| title_sort | xmagnet exascale mhd simulations of smbh feedback in galaxy groups and clusters overview and preliminary cluster results |
| topic | Galaxy clusters Galaxy jets Intracluster medium Magnetic fields Magnetohydrodynamical simulations |
| url | https://doi.org/10.3847/1538-4357/adde45 |
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