Thermal history of white dwarf pollutants

该项目旨在研究白色矮星Roche极限内星子从形成到潮汐破裂的热演化（分异和挥发损失），以探索形成过程（例如，（1）行星系统的年龄。我们模拟了原始微行星内部温度分布的演变，这些微行星没有经历热处理（例如，辐射衰变），通过对流扩散方程，以评估由恒星通量和/或潮汐加热触发的分化/挥发损失的参数空间。参数空间的大小表明放射性衰变是否是必不可少的分化和挥发分损失恒星演化过程中的分数。

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.