Progenitors of Magnetars and Core-collapse Supernovae in Binary Systems
Continuing the summer student project, I compare MESA models with different initial rotation, mass transfer, and tidal interactions, then track their core rotation and structure before collapse.
- ▪At ASROC 2026, we reported MESA models with donor masses of 20-65 solar masses, initial mass ratios of 0.5-0.8, and orbital periods of 8-18 days.
- ▪Compared core rotation before collapse in accretors undergoing chemically homogeneous evolution and those following standard evolution.
- ▪Tested tidal spin-up in parameterized post-common-envelope stripped-star models; the common-envelope phase itself was not simulated.
I run and analyze MESA binary-evolution models, compare rotational and structural histories across model assumptions, and interpret how angular-momentum transfer, tidal interaction, and mass loss affect the pre-collapse core.
- ▪Supported by an NSTC Undergraduate Research Grant (2025).
- ▪Presented at the 2025 and 2026 ASROC Annual Meetings and the 2026 TPS Annual Meeting.
- ▪First-author manuscript submitted to The Astrophysical Journal (2026), with Prof. Kuo-Chuan Pan.
Results & Analysis
At the 2026 ASROC meeting, we presented two modeled routes to rapidly rotating pre-collapse cores: compact mass-transfer products and tidal spin-up after a proposed common-envelope phase. In the post-common-envelope models, assumed orbital periods of 0.5 days or less produced strong core spin-up. The common-envelope phase itself was not simulated; these are predictions from a parameterized post-envelope setup.
Progenitors of Magnetars and Core-collapse Supernovae in Binary Systems
Advisor
Prof. Kuo-Chuan Pan
Period
Sep 2024 - Present
Overview
Continuing the summer student project, I compare MESA models with different initial rotation, mass transfer, and tidal interactions, then track their core rotation and structure before collapse.
- At ASROC 2026, we reported MESA models with donor masses of 20-65 solar masses, initial mass ratios of 0.5-0.8, and orbital periods of 8-18 days.
- Compared core rotation before collapse in accretors undergoing chemically homogeneous evolution and those following standard evolution.
- Tested tidal spin-up in parameterized post-common-envelope stripped-star models; the common-envelope phase itself was not simulated.
Individual contribution
I run and analyze MESA binary-evolution models, compare rotational and structural histories across model assumptions, and interpret how angular-momentum transfer, tidal interaction, and mass loss affect the pre-collapse core.
Research Record
- ▪Supported by an NSTC Undergraduate Research Grant (2025).
- ▪Presented at the 2025 and 2026 ASROC Annual Meetings and the 2026 TPS Annual Meeting.
- ▪First-author manuscript submitted to The Astrophysical Journal (2026), with Prof. Kuo-Chuan Pan.
Results & Analysis
At the 2026 ASROC meeting, we presented two modeled routes to rapidly rotating pre-collapse cores: compact mass-transfer products and tidal spin-up after a proposed common-envelope phase. In the post-common-envelope models, assumed orbital periods of 0.5 days or less produced strong core spin-up. The common-envelope phase itself was not simulated; these are predictions from a parameterized post-envelope setup.