Nonthermal Emissions from a Head–Tail Radio Galaxy in 3D Magnetohydrodynamic Simulations
We present magnetohydrodynamic simulations of a jet–wind interaction in a galaxy cluster and the radio to gamma-ray and neutrino emissions from this “head–tail galaxy.” Our simulation follows the evolution of cosmic-ray (CR) particle spectra with energy losses and stochastic turbulence acceleration....
| Main Authors: | , , , , |
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| Format: | Article |
| Language: | English |
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IOP Publishing
2023-01-01
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| Series: | The Astrophysical Journal |
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| Online Access: | https://doi.org/10.3847/1538-4357/acd338 |
| _version_ | 1797699413154463744 |
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| author | Takumi Ohmura Katsuaki Asano Kosuke Nishiwaki Mami Machida Haruka Sakemi |
| author_facet | Takumi Ohmura Katsuaki Asano Kosuke Nishiwaki Mami Machida Haruka Sakemi |
| author_sort | Takumi Ohmura |
| collection | DOAJ |
| description | We present magnetohydrodynamic simulations of a jet–wind interaction in a galaxy cluster and the radio to gamma-ray and neutrino emissions from this “head–tail galaxy.” Our simulation follows the evolution of cosmic-ray (CR) particle spectra with energy losses and stochastic turbulence acceleration. We find that the reacceleration is essential to explaining the observed radio properties of head–tail galaxies, in which the radio flux and spectral index do not drastically change. Our models suggest that hard X-ray emissions can be detected around the head–tail galaxy in the Perseus cluster by hard X-ray satellites, such as FORCE, and they will potentially constrain the acceleration efficiency. We also explore the origin of the collimated synchrotron threads, which have been found in some head–tail galaxies by recent high-quality radio observations. Thin and elongated flux tubes, connecting the two tails, are formed by strong backflows at an early phase. We find that these threads advect with the wind for over 300 Myr without disruption. The radio flux from the flux tubes is much lower than the typical observed flux. An efficient CR diffusion process along the flux tubes, however, may solve this discrepancy. |
| first_indexed | 2024-03-12T04:07:47Z |
| format | Article |
| id | doaj.art-4f1aeaf167a74af195083dc74c0afe24 |
| institution | Directory Open Access Journal |
| issn | 1538-4357 |
| language | English |
| last_indexed | 2024-03-12T04:07:47Z |
| publishDate | 2023-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj.art-4f1aeaf167a74af195083dc74c0afe242023-09-03T11:12:24ZengIOP PublishingThe Astrophysical Journal1538-43572023-01-0195117610.3847/1538-4357/acd338Nonthermal Emissions from a Head–Tail Radio Galaxy in 3D Magnetohydrodynamic SimulationsTakumi Ohmura0https://orcid.org/0000-0002-0040-8968Katsuaki Asano1https://orcid.org/0000-0001-9064-160XKosuke Nishiwaki2https://orcid.org/0000-0003-2370-0475Mami Machida3https://orcid.org/0000-0001-6353-7639Haruka Sakemi4https://orcid.org/0000-0002-4037-1346Institute for Cosmic Ray Research, The University of Tokyo , 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8582, Japan ; tohmura@icrr.u-tokyo.ac.jpInstitute for Cosmic Ray Research, The University of Tokyo , 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8582, Japan ; tohmura@icrr.u-tokyo.ac.jpInstitute for Cosmic Ray Research, The University of Tokyo , 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8582, Japan ; tohmura@icrr.u-tokyo.ac.jpDivision of Science, National Astronomical Observatory of Japan , 2-21-1 Osawa, Mitaka, Tokyo 181-8588, JapanGraduate School of Science and Engineering, Kagoshima University , 1-21-35 Korimoto, Kagoshima 890-0065, JapanWe present magnetohydrodynamic simulations of a jet–wind interaction in a galaxy cluster and the radio to gamma-ray and neutrino emissions from this “head–tail galaxy.” Our simulation follows the evolution of cosmic-ray (CR) particle spectra with energy losses and stochastic turbulence acceleration. We find that the reacceleration is essential to explaining the observed radio properties of head–tail galaxies, in which the radio flux and spectral index do not drastically change. Our models suggest that hard X-ray emissions can be detected around the head–tail galaxy in the Perseus cluster by hard X-ray satellites, such as FORCE, and they will potentially constrain the acceleration efficiency. We also explore the origin of the collimated synchrotron threads, which have been found in some head–tail galaxies by recent high-quality radio observations. Thin and elongated flux tubes, connecting the two tails, are formed by strong backflows at an early phase. We find that these threads advect with the wind for over 300 Myr without disruption. The radio flux from the flux tubes is much lower than the typical observed flux. An efficient CR diffusion process along the flux tubes, however, may solve this discrepancy.https://doi.org/10.3847/1538-4357/acd338Magnetohydrodynamical simulationsNon-thermal radiation sourcesExtragalactic radio sourcesRadio galaxiesCosmic rays |
| spellingShingle | Takumi Ohmura Katsuaki Asano Kosuke Nishiwaki Mami Machida Haruka Sakemi Nonthermal Emissions from a Head–Tail Radio Galaxy in 3D Magnetohydrodynamic Simulations The Astrophysical Journal Magnetohydrodynamical simulations Non-thermal radiation sources Extragalactic radio sources Radio galaxies Cosmic rays |
| title | Nonthermal Emissions from a Head–Tail Radio Galaxy in 3D Magnetohydrodynamic Simulations |
| title_full | Nonthermal Emissions from a Head–Tail Radio Galaxy in 3D Magnetohydrodynamic Simulations |
| title_fullStr | Nonthermal Emissions from a Head–Tail Radio Galaxy in 3D Magnetohydrodynamic Simulations |
| title_full_unstemmed | Nonthermal Emissions from a Head–Tail Radio Galaxy in 3D Magnetohydrodynamic Simulations |
| title_short | Nonthermal Emissions from a Head–Tail Radio Galaxy in 3D Magnetohydrodynamic Simulations |
| title_sort | nonthermal emissions from a head tail radio galaxy in 3d magnetohydrodynamic simulations |
| topic | Magnetohydrodynamical simulations Non-thermal radiation sources Extragalactic radio sources Radio galaxies Cosmic rays |
| url | https://doi.org/10.3847/1538-4357/acd338 |
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