Thermal history of white dwarf pollutants

本项目旨在研究白矮星罗氏极限内从形成到潮汐破坏的星子的热演化（分化和挥发损失），以探索行星系统的形成过程（如约束年龄）。我们通过平流-扩散方程模拟原始星子内部温度剖面的演化过程，以评估恒星通量和/或潮汐加热触发的微分/挥发损失参数空间。参数空间的大小表明了在恒星演化过程中放射成因衰变是否对分化和挥发物损失的比例至关重要。

This project aims at investigating the thermal evolution (differentiation and volatile loss) of planetesimals from formation until tidal disruption inside the Roche limit of the white dwarf, to probe the formation processes (e.g., constrain the age) of the planetary system. We simulate the evolution of the temperature profile inside primitive planetesimals experiencing no thermal processing (e.g., radiogenic decay), via advection-diffusion equation, to evaluate the parameter space of differentiation/volatile loss triggered by stellar flux and/or tidal heating. The size of the parameter space indicates whether radiogenic decay is essential for differentiation and the fraction of volatiles lost during stellar evolution.