标题： 食双星的物理性质。 第八。 多星系统 显示英文标题

标题： Physics Of Eclipsing Binaries. VIII. Multiple systems

摘要： 多恒星系统在O型和B型恒星中尤为常见。 为了准确描述它们的动力学，必须考虑各组成部分之间的相互作用。 在本工作中，我们介绍了Phoebe中的新动力学模型，该模型可以用于此目的。 n体模型基于Reboundx数值积分器，并考虑了相互扰动、扁率、相对论效应或光时效应。 初始条件可以设置为分层结构或两对几何结构。 为了进行比较，我们还提供了一个简化的开普勒模型。 测光计算与之前类似，包括成对组件（或质心，如果是分层结构）的洛希瓣变形，以及所有相互掩食。 如果观测时间跨度足够长，以至于扰动（进动、共振）在掩食时间或持续时间内表现出来，这将允许构建精度高一个数量级的恒星系统模型。 本草案指的是Phoebe的一个开发版本，可在https://github.com/miroslavbroz/phoebe2/tree/interferometry获取。 它尚未包含在官方的Phoebe仓库中！ 显示英文摘要

摘要： Multiple stellar systems are common especially among O and B stars. In order to accurately describe their dynamics, interactions among components must be accounted for. In this work, we describe the new dynamical model in Phoebe, which could be used just for this purpose. The n-body model is based on the Reboundx numerical integrator and accounts for mutual perturbations, oblateness, relativistic effects, or light-time effects. The initial conditions can be set up as hierarchical or two-pairs geometry. For comparison purposes, we also provide a simplified keplerian model. Photometric computations work similarly as before, with Roche distortions for pairs of components (or for centres of mass, if hierarchical), and all mutual eclipses. If the time span of observations is long enough, so that perturbations (precession, resonances) are manifested in eclipse timings or durations, this allows to construct order-of-magnitude more precise models of stellar systems. This draft refers to a development version of Phoebe, available at https://github.com/miroslavbroz/phoebe2/tree/interferometry . It is not yet included in the official Phoebe repository!