Using nebular spectra to reveal the progenitor and explosion mechanism of core-collpase supernovae
| Project/Area Number |
20J23342
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| Research Category |
Grant-in-Aid for JSPS Fellows
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| Allocation Type | Single-year Grants |
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| Section | 国内 |
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| Review Section |
Basic Section 16010:Astronomy-related
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| Research Institution | Kyoto University |
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Principal Investigator |
方 其亮 京都大学, 理学研究科, 特別研究員(DC1)
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| Project Period (FY) |
2020-04-24 – 2023-03-31
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| Project Status |
Granted (Fiscal Year 2022)
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| Budget Amount *help |
¥2,800,000 (Direct Cost: ¥2,800,000)
Fiscal Year 2022: ¥900,000 (Direct Cost: ¥900,000)
Fiscal Year 2021: ¥900,000 (Direct Cost: ¥900,000)
Fiscal Year 2020: ¥1,000,000 (Direct Cost: ¥1,000,000)
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| Keywords | Supernvoa / Transient source / Spectroscopy / Spectrum |
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| Outline of Research at the Start |
This research will use a method that measures the mass of a star, developed by our previous work, and powerful telescopes, to investigate the physics process when the star explodes at the end of its life. With this method, we can also investigate how a star loss its weight before the explosion.
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| Outline of Annual Research Achievements |
The relation between the progenitor mass and the kinetic energy of the explosion is a key toward revealing the explosion mechanism of stripped-envelope (SE) core-collapse (CC) supernovae (SNe). In this work, we present a method to derive this relation using the nebular spectra of SESNe, based on the correlation between [O I]/[Ca II], which measures the progenitor mass, and [O I] width, which measures the expansion velocity of the ejecta. Using hydrodynamic simulations, we trigger explosions with different kinetic energy and progenitor mass. The models are compared with observation. We find the mass-energy scaling relation required to explain the observed mass-velocity correlation. We further demonstrate helium-rich and helium-deficient SNe follow the same mass-energy scaling relation.
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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
We have successfully performed hydrodynamic models with different progenitor mass and kinetic energy. We further build up the method to connect the properties of the models with the observed quantities, including the scaling relation between the oxygen mass and [O I]/[Ca II] ratio, and the construction of the [O I] profile from the ejecta structure. These models and the practice can be applied in future works. A manuscript is now in preparation.
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| Strategy for Future Research Activity |
In the current work, the mass-energy relation is built up based on the nebular spectroscopy, biasing toward the dense inner core. Our future work aims to compare the result in this work with the ejecta mass-energy relation built up based on the early phase observation, which measures the properties of the outermost region. The systematic comparison of the late phase and early phase observation provides us the unique chance to scan through the ejecta from outer to inner region (as computed tomography, or CT), which is crucial to understand the ejecta structure.
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Report
(2 results)
Research Products
(3 results)
