| Project/Area Number |
22KF0246
|
|---|
| Project/Area Number (Other) |
22F22327 (2022)
|
|---|
| Research Category |
Grant-in-Aid for JSPS Fellows
|
| Allocation Type | Multi-year Fund (2023)
Single-year Grants (2022) |
|---|
| Section | 外国 |
|---|
| Review Section |
Basic Section 16010:Astronomy-related
|
|---|
| Research Institution | Osaka University |
|---|
Principal Investigator |
井上 芳幸 大阪大学, 大学院理学研究科, 准教授 (70733989)
|
|---|
| 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
|
|---|
| Project Period (FY) |
2023-03-08 – 2025-03-31
|
| Project Status |
Granted (Fiscal Year 2023)
|
| 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)
|
|---|
| Keywords | Hadronic interactions / galaxy evolution / cosmic rays / magnetic fields / Cosmic rays / hadronic interactions |
|---|
| 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。
|
| Outline of Annual Research Achievements |
Research in FY2023 has focused on constructing detailed microphysical models and emission signatures from the physical media conditions expected in starburst galaxies and the intergalactic medium. This has put focus on ultra-high-energy particle scattering and propagation in cosmological magnetic field structures, and intermediate to high energy particle interactions in cosmological and astrophysical radiation and density fields. Some of these microphysical interaction models have been interfaced into magnetohydrodynamical simulation codes, with validation of these code implementations still ongoing.
|
| Current Status of Research Progress |
Current Status of Research Progress
3: Progress in research has been slightly delayed.
Reason
Progress is generally running according to plan, however the implementation of cosmic ray interaction microphysics into numerical codes has been slower than expected. This is because of (1) a need to await new hadronic interaction models based on interpolated functions from new hadronic code outputs to ensure the treatment of secondary lepton production near interaction thresholds is robust (Afrag version 2.02); (2) unexpected additional work required to prepare an existing codebase (in FLASH4) for the additional hadronic interaction functionality required. It has also been decided to implement the relevant physics into another open-source code base (Athena++) to allow for more flexible scientific application and usage, which will require additional time in FY2024.
|
| Strategy for Future Research Activity |
Detailed cosmic ray interaction microphysics models have been developed and are currently being implemented and validated in magnetohydrodynamical codebases. Application of these microphysical treatments of cosmic ray processes to cosmological filaments, galaxy bubbles, compact groups of galaxies and high energy gamma-ray backgrounds will be the main focus for this research programme during FY 2024 as the project moves into its final stages. While some delays have been encountered, sufficient provision for such delays were included in the original plan to ensure the planned research objectives can still be met within the remaining timeline.
|
