| Project/Area Number |
23KJ0392
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| Research Category |
Grant-in-Aid for JSPS Fellows
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| Allocation Type | Multi-year Fund |
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| Section | 国内 |
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| Review Section |
Basic Section 15010:Theoretical studies related to particle-, nuclear-, cosmic ray and astro-physics
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| Research Institution | The University of Tokyo |
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Principal Investigator |
ZHONG Yici 東京大学, 理学系研究科, 特別研究員(DC2)
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| Project Period (FY) |
2023-04-25 – 2025-03-31
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| Project Status |
Discontinued (Fiscal Year 2023)
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| Budget Amount *help |
¥2,800,000 (Direct Cost: ¥2,800,000)
Fiscal Year 2024: ¥1,400,000 (Direct Cost: ¥1,400,000)
Fiscal Year 2023: ¥1,400,000 (Direct Cost: ¥1,400,000)
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| Keywords | compact object / stellar wind |
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| Outline of Research at the Start |
The purpose of this research is to understand the missing link between core collapse supernova explosion and neutron star formation - observed neutron star diversity by first principle studies. we will numerically construct realistic outflow from neutron stars with various surface environments, rotation period and magnetic field configurations, and precisely model the interaction between this outflow and fallback matter together with their imprints on the observation signal, such as pulsar wind nebulae (PWNe), light curve and radiation spectrum.
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| Outline of Annual Research Achievements |
Our research, inspired by Yici Zhong et al. (2021), focuses on simulating magnetic-driven winds from compact objects, particularly white dwarfs, employing magnetohydrodynamics (MHD) studies. Initially, we reproduce the adiabatic wind solution to approximate physical conditions around white dwarfs. Then, we introduce magnetic fields to initiate magnetic-driven winds. We investigate various wind adiabatic indices, examining equatorial plane profiles and the scaling of wind velocity at infinity with temperature. For magnetic-driven winds, we establish an internal energy floor to address regions dominated by magnetic energy, tracking its time evolution separately. We analyze the sonic radius, Alfven radius, and the dependence of open magnetic flux on radii at different latitudes. Our findings confirm an anisotropic wind structure with the formation of equatorial current sheets. Additionally, we discuss the spin evolution of the white dwarf merger remnant WD J005311 in Yici Zhong et al. (2024).
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| Current Status of Research Progress |
Current Status of Research Progress
1: Research has progressed more than it was originally planned.
Reason
The work supported by this grant has been published on ApJ 963 26 (2024), together with another co-author paper Phys. Rev. D 108, 043521 (2023). There are two presentations (all peer reviewed) in international conference that are supported by this grant as well: "Spindown of Pulsars Interacting with Companion Winds", The 32nd Texas Symposium on Relativistic Astrophysics, Shanghai, China (2023.12) and "Spindown of Pulsars Interacting with Companion Winds: Implications for the Double Pulsar PSR J0737-3039", poster session in HEPRO VIII : High Energy
Phenomena in Relativistic Outflows, Paris, France (2023.10).
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| Strategy for Future Research Activity |
My research project will continue to advance in several key directions. Firstly, I will persist in studying the stellar wind emanating from compact objects through the utilization of high-performance simulations. This will enable me to delve deeper into the intricacies of wind dynamics and their interactions with surrounding environments. Secondly, my primary emphasis will be on exploring the long-term evolution of the magnetic fields of accreting neutron stars. By conducting detailed investigations into the complex interplay between accretion processes and magnetic field evolution, I aim to uncover insights into the behavior and characteristics of these systems over extended timescales. Furthermore, I intend to augment my numerical simulations by incorporating radiative transfer mechanisms and accounting for general relativistic effects. By doing so, I seek to capture the full complexity of the physical phenomena at play, allowing for a more comprehensive understanding of the observed phenomena in neutron star environments.
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