Accretion Flow Morphology in Numerical Simulations of Black Holes from the ngEHT Model Library: The Impact of Radiation Physics
In the past few years, the Event Horizon Telescope (EHT) has provided the first-ever event horizon-scale images of the supermassive black holes (BHs) M87∗ and Sagittarius A∗ (Sgr A∗ ). The next-generation EHT project is an extension of the EHT array that promises larger angular resolution and higher...
| Autores: | , , , , , , , , , , , , , , , , , , , , |
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| Tipo de recurso: | artículo |
| Estado: | Versión publicada |
| Fecha de publicación: | 2023 |
| País: | España |
| Institución: | Consejo Superior de Investigaciones Científicas (CSIC) |
| Repositorio: | DIGITAL.CSIC. Repositorio Institucional del CSIC |
| OAI Identifier: | oai:digital.csic.es:10261/330557 |
| Acceso en línea: | http://hdl.handle.net/10261/330557 |
| Access Level: | acceso abierto |
| Palabra clave: | Black holes General relativity Accretion Relativistic jets Very-long-baseline interferometry ddc:520 |
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oai:digital.csic.es:10261/330557 |
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Accretion Flow Morphology in Numerical Simulations of Black Holes from the ngEHT Model Library: The Impact of Radiation Physics Chatterjee, Koushik Chael, Andrew Tiede, Paul Mizuno, Yosuke Emami, Razieh Fromm, Christian Ricarte, Angelo Blackburn, Lindy Roelofs, Freek Johnson, Michael D. Doeleman, Sheperd S. Arras, Philipp Fuentes, Antonio Knollmüller, Jakob Kosogorov, Nikita Lindahl, Greg Müller, Hendrik Patel, Nimesh Raymond, Alexander W. Traianou, E. Vega, Justin Black holes General relativity Accretion Relativistic jets Very-long-baseline interferometry ddc:520 In the past few years, the Event Horizon Telescope (EHT) has provided the first-ever event horizon-scale images of the supermassive black holes (BHs) M87∗ and Sagittarius A∗ (Sgr A∗ ). The next-generation EHT project is an extension of the EHT array that promises larger angular resolution and higher sensitivity to the dim, extended flux around the central ring-like structure, possibly connecting the accretion flow and the jet. The ngEHT Analysis Challenges aim to understand the science extractability from synthetic images and movies to inform the ngEHT array design and analysis algorithm development. In this work, we compare the accretion flow structure and dynamics in numerical fluid simulations that specifically target M87∗ and Sgr A∗, and were used to construct the source models in the challenge set. We consider (1) a steady-state axisymmetric radiatively inefficient accretion flow model with a time-dependent shearing hotspot, (2) two time-dependent single fluid general relativistic magnetohydrodynamic (GRMHD) simulations from the H-AMR code, (3) a two-temperature GRMHD simulation from the BHAC code, and (4) a two-temperature radiative GRMHD simulation from the KORAL code. We find that the different models exhibit remarkably similar temporal and spatial properties, except for the electron temperature, since radiative losses substantially cool down electrons near the BH and the jet sheath, signaling the importance of radiative cooling even for slowly accreting BHs such as M87∗. We restrict ourselves to standard torus accretion flows, and leave larger explorations of alternate accretion models to future work. © 2023 by the authors. Licensee MDPI, Basel, Switzerland. We thank the National Science Foundation (AST-1716536, AST-1935980 and AST-2034306) and the Gordon and Betty Moore Foundation (GBMF-10423) for financially supporting this work. This work was supported in part by the Black Hole Initiative, which is funded by grants from the John Templeton Foundation (JTF-61497) and the Gordon and Betty Moore Foundation (GBMF-8273) to Harvard University. K.C. is also supported in part by the Black Hole PIRE program (NSF grant OISE-1743747). R.E. acknowledges the support by the Institute for Theory and Computation at the Center for Astrophysics as well as grant numbers 21-atp21-0077, NSF AST-1816420, and HST-GO-16173.001-A for very generous supports. H.M. received financial support for this research from the International Max Planck Research School (IMPRS) for Astronomy and Astrophysics at the Universities of Bonn and Cologne. This research is supported by the DFG research grant “Jet physics on horizon scales and beyond” (Grant No. FR 4069/2-1), the ERC synergy grant “BlackHoleCam: Imaging the Event Horizon of Black Holes” (Grant No. 610058), and ERC advanced grant “JETSET: Launching, propagation and emission of relativistic jets from binary mergers and across mass scales” (Grant No. 884631). J.K. acknowledges funding by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) under Germany´s Excellence Strategy—EXC 2094—390783311. Y.M. is supported by the National Natural Science Foundation of China (No. 12273022) and the Shanghai pilot program of international scientists for basic research (No. 22JC1410600). Peer reviewed Multidisciplinary Digital Publishing Institute http://hdl.handle.net/10261/330557 |
| title |
Accretion Flow Morphology in Numerical Simulations of Black Holes from the ngEHT Model Library: The Impact of Radiation Physics |
| spellingShingle |
Accretion Flow Morphology in Numerical Simulations of Black Holes from the ngEHT Model Library: The Impact of Radiation Physics Chatterjee, Koushik Black holes General relativity Accretion Relativistic jets Very-long-baseline interferometry ddc:520 |
| title_short |
Accretion Flow Morphology in Numerical Simulations of Black Holes from the ngEHT Model Library: The Impact of Radiation Physics |
| title_full |
Accretion Flow Morphology in Numerical Simulations of Black Holes from the ngEHT Model Library: The Impact of Radiation Physics |
| title_fullStr |
Accretion Flow Morphology in Numerical Simulations of Black Holes from the ngEHT Model Library: The Impact of Radiation Physics |
| title_full_unstemmed |
Accretion Flow Morphology in Numerical Simulations of Black Holes from the ngEHT Model Library: The Impact of Radiation Physics |
| title_sort |
Accretion Flow Morphology in Numerical Simulations of Black Holes from the ngEHT Model Library: The Impact of Radiation Physics |
| author |
Chatterjee, Koushik |
| author_facet |
Chatterjee, Koushik Chael, Andrew Tiede, Paul Mizuno, Yosuke Emami, Razieh Fromm, Christian Ricarte, Angelo Blackburn, Lindy Roelofs, Freek Johnson, Michael D. Doeleman, Sheperd S. Arras, Philipp Fuentes, Antonio Knollmüller, Jakob Kosogorov, Nikita Lindahl, Greg Müller, Hendrik Patel, Nimesh Raymond, Alexander W. Traianou, E. Vega, Justin |
| author_role |
author |
| author2 |
Chael, Andrew Tiede, Paul Mizuno, Yosuke Emami, Razieh Fromm, Christian Ricarte, Angelo Blackburn, Lindy Roelofs, Freek Johnson, Michael D. Doeleman, Sheperd S. Arras, Philipp Fuentes, Antonio Knollmüller, Jakob Kosogorov, Nikita Lindahl, Greg Müller, Hendrik Patel, Nimesh Raymond, Alexander W. Traianou, E. Vega, Justin |
| author2_role |
author author author author author author author author author author author author author author author author author author author author |
| topic |
Black holes General relativity Accretion Relativistic jets Very-long-baseline interferometry ddc:520 |
| topic_facet |
Black holes General relativity Accretion Relativistic jets Very-long-baseline interferometry ddc:520 |
| description |
In the past few years, the Event Horizon Telescope (EHT) has provided the first-ever event horizon-scale images of the supermassive black holes (BHs) M87∗ and Sagittarius A∗ (Sgr A∗ ). The next-generation EHT project is an extension of the EHT array that promises larger angular resolution and higher sensitivity to the dim, extended flux around the central ring-like structure, possibly connecting the accretion flow and the jet. The ngEHT Analysis Challenges aim to understand the science extractability from synthetic images and movies to inform the ngEHT array design and analysis algorithm development. In this work, we compare the accretion flow structure and dynamics in numerical fluid simulations that specifically target M87∗ and Sgr A∗, and were used to construct the source models in the challenge set. We consider (1) a steady-state axisymmetric radiatively inefficient accretion flow model with a time-dependent shearing hotspot, (2) two time-dependent single fluid general relativistic magnetohydrodynamic (GRMHD) simulations from the H-AMR code, (3) a two-temperature GRMHD simulation from the BHAC code, and (4) a two-temperature radiative GRMHD simulation from the KORAL code. We find that the different models exhibit remarkably similar temporal and spatial properties, except for the electron temperature, since radiative losses substantially cool down electrons near the BH and the jet sheath, signaling the importance of radiative cooling even for slowly accreting BHs such as M87∗. We restrict ourselves to standard torus accretion flows, and leave larger explorations of alternate accretion models to future work. © 2023 by the authors. Licensee MDPI, Basel, Switzerland. |
| publishDate |
2023 |
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article |
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publishedVersion |
| url |
http://hdl.handle.net/10261/330557 |
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openAccess |
| publisher |
Multidisciplinary Digital Publishing Institute |
| institution |
Consejo Superior de Investigaciones Científicas (CSIC) |
| collection |
DIGITAL.CSIC. Repositorio Institucional del CSIC |
| reponame_str |
DIGITAL.CSIC. Repositorio Institucional del CSIC |
| instname_str |
Consejo Superior de Investigaciones Científicas (CSIC) |
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1878432282751008768 |
| publishDateSort |
2023 |
| author_browse |
Arras, Philipp Blackburn, Lindy Chael, Andrew Chatterjee, Koushik Doeleman, Sheperd S. Emami, Razieh Fromm, Christian Fuentes, Antonio Johnson, Michael D. Knollmüller, Jakob Kosogorov, Nikita Lindahl, Greg Mizuno, Yosuke Müller, Hendrik Patel, Nimesh Raymond, Alexander W. Ricarte, Angelo Roelofs, Freek Tiede, Paul Traianou, E. Vega, Justin |
| publisherStr |
Multidisciplinary Digital Publishing Institute |
| score |
6,9303427 |