论文标题
朝着热四倍系统HD 93206 = QZCarinæ的一致模型：II。 N体模型
Towards a consistent model of the hot quadruple system HD 93206 = QZ Carinæ: II. N-body model
论文作者
论文摘要
HD 93206是早期型巨大的恒星系统，由通过直接成像（AB，AD，B，C，C，D）解决的组件以及紧凑的子系统（AA1，AA2，AC1，AC2）组成。它的几何形状已经根据广泛的光度，光谱和干涉观测确定。但是，基本的绝对参数仍然不够得知。我们使用先进的N体模型来说明四个关闭组件之间的所有相互重力扰动，以及所有观察数据类型，包括：天文学，径向速度，Eclipse时正时变化，平方可见性，闭合相，三重产物，归一化光谱和光谱元素分布（SED）。相应的模型具有38个自由参数，即三组轨道元素，组件质量及其基本辐射属性（$ t $，$ \ log g $，$ v _ {\ rm rot} $）。我们修改了QZ汽车的基本参数，如下所示。对于具有名义灭绝系数$ r_v \ equiv a_v/e（b-v）= 3.1 $的模型，最佳拟合质量为$ m_1 = 26.1 = 26.1 \，m _ {\ rm s} $，$ m_2 = 32.3 = 32.3 \ \，m _ { s} $，$ m_4 = 8.8 \，m _ {\ rm s} $，不确定性为$ 2 \，m _ {\ rm s} $，而系统距离$ d =（2800 \ pm 100）\，{\ rm pc} $。在替代模型中，我们增加了RV和TTV观测的权重并放松了SED约束，因为灭绝可能与$ R_V \ sim 3.4 $是异常的，距离较小，$ d =（2450 \ pm 100）\，{\ rm pc} $。这将与Collinder 228群集的相对应。独立地，通过sed的德雷德登（SED）证实，这只是与早期类型的分类一致（aa1的o9.7ib，o8iii for ac1）。未来的建模还应说明AC2组件周围的积聚盘。
HD 93206 is early-type massive stellar system, composed of components resolved by direct imaging (Ab, Ad, B, C, D) as well as a compact sub-system (Aa1, Aa2, Ac1, Ac2). Its geometry was already determined on the basis of extensive photometric, spectroscopic and interferometric observations. However, the fundamental absolute parameters are still not known precisely enough. We use an advanced N-body model to account for all mutual gravitational perturbations among the four close components, and all observational data types, including: astrometry, radial velocities, eclipse timing variations, squared visibilities, closure phases, triple products, normalized spectra, and spectral-energy distribution (SED). The respective model has 38 free parameters, namely three sets of orbital elements, component masses, and their basic radiative properties ($T$, $\log g$, $v_{\rm rot}$). We revised the fundamental parameters of QZ Car as follows. For a model with the nominal extinction coefficient $R_V \equiv A_V/E(B-V) = 3.1$, the best-fit masses are $m_1 = 26.1\,M_{\rm S}$, $m_2 = 32.3\,M_{\rm S}$, $m_3 = 70.3\,M_{\rm S}$, $m_4 = 8.8\,M_{\rm S}$, with uncertainties of the order of $2\,M_{\rm S}$, and the system distance $d = (2800\pm 100)\,{\rm pc}$. In an alternative model, where we increased the weights of RV and TTV observations and relaxed the SED constraints, because extinction can be anomalous with $R_V \sim 3.4$, the distance is smaller, $d = (2450\pm 100)\,{\rm pc}$. This would correspond to that of Collinder 228 cluster. Independently, this is confirmed by dereddening of the SED, which is only then consistent with the early-type classification (O9.7Ib for Aa1, O8III for Ac1). Future modelling should also account for an accretion disk around Ac2 component.
