Feedback interactions between galaxies in compact groups: photonic, leptonic and hadronic processes
| Project/Area Number |
22KF0246
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| Project/Area Number (Other) |
22F22327 (2022)
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| Research Category |
Grant-in-Aid for JSPS Fellows
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| Allocation Type | Multi-year Fund (2023)
Single-year Grants (2022) |
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| Section | 外国 |
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| Review Section |
Basic Section 16010:Astronomy-related
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| Research Institution | Osaka University |
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Principal Investigator |
井上 芳幸 大阪大学, 大学院理学研究科, 准教授 (70733989)
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| Co-Investigator(Kenkyū-buntansha) |
OWEN ELLIS 大阪大学, 大学院理学研究科, 外国人特別研究員
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| Project Period (FY) |
2023-03-08 – 2025-03-31
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| Project Status |
Granted (Fiscal Year 2023)
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| Budget Amount *help |
¥2,300,000 (Direct Cost: ¥2,300,000)
Fiscal Year 2024: ¥600,000 (Direct Cost: ¥600,000)
Fiscal Year 2023: ¥1,200,000 (Direct Cost: ¥1,200,000)
Fiscal Year 2022: ¥500,000 (Direct Cost: ¥500,000)
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| Keywords | Cosmic rays / hadronic interactions / magnetic fields / galaxy evolution |
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| Outline of Research at the Start |
物理学における重要課題の一つである宇宙史解明において、銀河の形成・進化過程の理解は必要不可欠である。近年、銀河宇宙線の役割が重要な研究テーマとなっている。特に、銀河は形成進化過程において互いに相互作用を起こすため、孤立銀河だけでなく、銀河集団での宇宙線の役割も理解する必要がある。本研究課題においては、銀河間距離が近い故に銀河間相互作用が強いコンパクト 銀河群における宇宙線の役割を解明する。そして、本成果を銀河進化の枠組み全体へと適応するこ とを目指す。
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| Outline of Annual Research Achievements |
During the first 4 months of the research program, this project led to the publication of 1 paper (Lin, Yang & Owen, 2023), and the submission of 1 further paper (Owen, Han & Wu, submitted to Phys. Rev. D). These concern the development of cosmic ray interactions and the effects of the magnetohydrodynamics (MHD) of diffuse astrophysical structures around galaxies, and cosmic ray propagation microphysics in magnetic fields, respectively. Additionally, 7 oral presentations (4 invited) were delivered in departmental/group seminars and national/international conferences relating to results obtained during the initial stages of this project.
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| Current Status of Research Progress |
Current Status of Research Progress
2: Research has progressed on the whole more than it was originally planned.
Reason
Focus during this initial stage of the project was placed on resolving the cosmic ray interaction and propagation microphysics in magnetized, multiphase diffuse astrophysical environments, particularly within flows and large-scale structures. Building-up the microphysical picture of cosmic ray physics is an essential foundation before robust macroscopic models can be constructed on galactic scales. The following specific developments have been completed:
(1)A large-scale scattering formulation of cosmic ray propagation and interaction has been developed. This was applied to large scale magnetic fields and the propagation of ultrahigh-energy cosmic rays as a demonstration, but the formation is general for inhomogeneous magnetic field structures and will be applied to the science goals of this project. The first demonstration study has been submitted for publication at Physical Review D and is currently undergoing peer review.
(2)A microphysical hadronic cosmic ray interaction code has been constructed using state-of-the art interaction cross sections. This allows for a full treatment of spectrally resolved hadronic cosmic rays, self-consistent production of secondary leptonic cosmic rays and a complete treatment of their momentum evolution. This has been implemented in an adaptive mesh refined MHD code (FLASH). Code demonstration and validation runs will soon begin.
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| Strategy for Future Research Activity |
As of April 2023, the project is progressing to schedule. The immediate technical priorities to be developed during the next stage of the project (FY 2023) are:
(1) Development of robust treatment of magnetized cloud flow interaction; development of a multi-phase framework for a galactic flow, properly accounting for the non-thermal driving history and cosmic ray engagement at the cloud/flow boundary. (2) Validation of self-consistent hadronic cosmic ray code model in MHD simulations of galactic bubbles and outflows. First science demonstration case. (3) Compute gamma-ray emission from hadronic processes multi-phase flows and determine its evolutionary progression under different flow driving physics and boundary conditions. (4) Calculation of dust grain properties under cosmic ray collisions. Application to 1-dimensional models of galactic outflows and circum-galactic environments. Application to a simple cosmic ray advection/diffusion model of a galaxy to obtain testable mid-infrared observables for cosmic ray activity in galactic ecosystems.
Application of cosmic ray propagation and interaction models to compact galaxy group environments will proceed in FY 2024, after the above microphysical treatments have been developed.
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Report
(1 results)
Research Products
(5 results)
