论文标题
单星序后序列系统中的晶粒尺寸生存阈值
The grain size survival threshold in one-planet post-main-sequence exoplanetary systems
论文作者
论文摘要
在进化的巨大分支阶段，尘埃，谷物，巨石，小行星和主要行星的尺寸分布和轨道结构决定了最终碎屑的优势和可观察性，这些碎屑的大小和可观察性围绕着白色矮人，并用金属用金属污染了大气。在这里，我们利用了一行巨型分支系统中的光载平面限制了三体问题，以表征晶粒的轨道为母星的光度和质量发生巨大变化。我们对整个巨大分支演化的位置和能量的函数进行详细的动态分析（碰撞，逃生或有限）的特征。我们发现，对于主要序列质量为200万美元_ {\ odot} $的恒星，巨大的分支进化，结合一个行星的存在，无处不在的触发器散发出小于1 mm的谷物中，同时使谷物大于大约5 cm的谷物与恒星结合。该结果适用于具有陆地或巨型行星的系统，在很大程度上与行星的位置无关，并有助于建立一个辐射尺寸的阈值，以逃避巨型分支行星系统中小颗粒的逃生。
The size distribution and orbital architecture of dust, grains, boulders, asteroids, and major planets during the giant branch phases of evolution dictate the preponderance and observability of the eventual debris, which have been found to surround white dwarfs and pollute their atmospheres with metals. Here, we utilize the photogravitational planar restricted three-body problem in one-planet giant branch systems in order to characterize the orbits of grains as the parent star luminosity and mass undergo drastic changes. We perform a detailed dynamical analysis of the character of grain orbits (collisional, escape, or bounded) as a function of location and energy throughout giant branch evolution. We find that for stars with main-sequence masses of $2.0M_{\odot}$, giant branch evolution, combined with the presence of a planet, ubiquitously triggers escape in grains smaller than about 1 mm, while leaving grains larger than about 5 cm bound to the star. This result is applicable for systems with either a terrestrial or giant planet, is largely independent of the location of the planet, and helps establish a radiative size threshold for escape of small particles in giant branch planetary systems.
