年轻双星Haro 1-14 C的质量和距离
Refined masses and distance of the young binary Haro 1-14 C
摘要：
我们的目标是细化的动力学质量的低质量前主序星二进制哈罗1-14 C的单个组件。我们结合的初步轨道的数据与新的干涉观测获得的4个8米望远镜的甚大望远镜干涉仪。一级和二级组分的推导质量分别为$M_a=0.905\pm0.043\,\Msun$和$M_b=0.308\pm0.011\,\Msun$。这比初始轨道的不确定性好大约五倍。此外，更大质量的可能性现在被安全地抛弃了。新的动力学距离$d=96\pm\,9\,$ pc小于蛇夫座核心的距离，其显著性为$2.6\,σ$。拟合光谱能量分布得到$ϕ_a=0.13\pm0.01\mas$和$ϕ_b=0.10\pm0.01\mas$的表观直径（对应于$\Ra=1.50\,\Rsun$和$\Rb=1.13\,\Rsun$）和$A_v\approx1.75$的可见消光。虽然修正后的轨道有一个接近边缘的几何形状，但该系统不太可能是一个长周期的食双星。Haro~1- 14 C的次级恒星是少数几颗动力学质量和距离都精确测定的低质量主序星之一。
英文摘要：
We aim to refine the dynamical masses of the individual component of the low-mass pre-main sequence binary Haro 1-14 C. We combine the data of the preliminary orbit presented previously with new interferometric observations obtained with the four 8m telescopes of the Very Large Telescope Interferometer. The derived masses are $M_a=0.905\pm0.043\,\Msun$ and $M_b=0.308\pm0.011\,\Msun$ for the primary and secondary components, respectively. This is about five times better than the uncertainties of the preliminary orbit. Moreover, the possibility of larger masses is now securely discarded. The new dynamical distance, $d=96\pm\,9\,$pc, is smaller than the distance to the Ophiuchus core with a significance of $2.6\,σ$. Fitting the spectral energy distribution yields apparent diameters of $ϕ_a=0.13\pm0.01\mas$ and $ϕ_b=0.10\pm0.01\mas$ (corresponding to $\Ra=1.50\,\Rsun$ and $\Rb=1.13\,\Rsun$) and a visual extinction of $A_v\approx1.75$. Although the revised orbit has a nearly edge-on geometry, the system is unlikely to be a long-period eclipsing binary. The secondary in Haro~1-14C is one of the few low-mass, pre-main sequence stars with an accurately determined dynamical mass and distance.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
