发表机构
University of Nevada, Las Vegas; Nevada Center for Astrophysics, University of Nevada, Las Vegas（内华达大学拉斯维加斯分校; 内华达天体物理中心，内华达大学拉斯维加斯分校）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究利用N体模拟和尘埃凝聚模型，探究不同碳氧比下系外行星的形成，发现体密度可区分富硅与富碳行星，但单独使用不可靠。
AI 中文摘要
研究表明，围绕具有高碳氧比（C/O）恒星的原始行星盘可以产生以碳为主而非以硅为主成分的类地行星。虽然先前的工作研究了这些盘的演化及其内部形成的行星，但没有任何研究详细分析这些盘表面密度分布的差异如何影响系外行星系统的架构以及铁和亲铁元素含量。在此，我们提出一项新研究，利用N体积分器REBOUND和顺序尘埃凝聚模型的数据，模拟不同C/O比系统中行星的形成。我们发现，体密度可用于区分富硅行星和富碳行星，尽管它本身可能不是一个可靠的指标。
英文摘要
Studies suggest that protoplanetary disks around stars with high carbon-to-oxygen (C/O) ratios can produce terrestrial planets with carbon-dominated compositions instead of silicon-dominated ones. While previous work studied the evolution of these disks and the planets that form within them, none analyze in detail how the differences in the surface density profiles of these disks could affect the architectures and iron and siderophile contents of exoplanetary systems. Here, we present a new study that uses the N-body integrator REBOUND and data from a sequential dust condensation model to simulate the formation of planets in systems with varying C/O ratios. We find that bulk density could be used to distinguish between silicon-rich and carbon-rich planets, though it may not be a reliable metric on its own.
Comments14 pages, 11 figures, 9 Tables, Submitted to the Open Journal of Astrophysics
