Be+ sdO双星Phi Persei的光谱和空间成像
Spectral and spatial imaging of the Be+sdO binary phi Persei
摘要：
快速旋转的Be星英仙座φ是通过质量和角动量转移从一个现在剥离下来的热亚矮星伴星旋转起来的。在这里，我们提出了第一个高角分辨率图像的phi英仙座可能的新能力，在长基线干涉在近红外和可见光波长。我们用CHARA阵列的MIRC和VEGA仪器观测了英仙座φ。进行了额外的仅限MIRC的观测，以跟踪伴星的轨道运动，并将这些观测与两颗恒星的新的和现有的径向速度测量相结合，以得出完整的轨道要素和距离。在每个观测时期的近红外数据中，热亚矮星伴星都被清楚地探测到，H波段的通量贡献为1.5%，限制拟合表明其通量贡献在可见光中上升到3.3%。结合天体测量和径向速度测量，确定了一个新的双星轨道解。计算出Be主星和次矮星的质量分别为9.6 ± 0.3Msol和1.2 ± 0.2Msol。推断的距离（186 +- 3 pc），运动学性质，和进化状态是一致的，在阿尔法Per集群中的phi英仙座成员。从集群的年龄，我们推导出显着的初始质量和演化的质量转移过程，改造了英仙座的phi二元系统的限制。干涉测量数据对Be盘的伸长、方向和运动学有很强的约束，并且盘的角动量矢量与轨道角动量矢量共同对齐并具有相同的旋转方向。VEGA的可见光连续谱数据表明Be星本身的形状是细长的，这是由于快速旋转、星周盘对光球的部分遮蔽以及明亮的内盘的通量的综合影响。
英文摘要：
The rapidly rotating Be star phi Persei was spun up by mass and angular momentum transfer from a now stripped-down, hot subdwarf companion. Here we present the first high angular resolution images of phi Persei made possible by new capabilities in longbaseline interferometry at near-IR and visible wavelengths. We observed phi Persei with the MIRC and VEGA instruments of the CHARA Array. Additional MIRC-only observations were performed to track the orbital motion of the companion, and these were fit together with new and existing radial velocity measurements of both stars to derive the complete orbital elements and distance. The hot subdwarf companion is clearly detected in the near-IR data at each epoch of observation with a flux contribution of 1.5% in the H band, and restricted fits indicate that its flux contribution rises to 3.3% in the visible. A new binary orbital solution is determined by combining the astrometric and radial velocity measurements. The derived stellar masses are 9.6+-0.3Msol and 1.2+-0.2Msol for the Be primary and subdwarf secondary, respectively. The inferred distance (186 +- 3 pc), kinematical properties, and evolutionary state are consistent with membership of phi Persei in the alpha Per cluster. From the cluster age we deduce significant constraints on the initial masses and evolutionary mass transfer processes that transformed the phi Persei binary system. The interferometric data place strong constraints on the Be disk elongation, orientation, and kinematics, and the disk angular momentum vector is coaligned with and has the same sense of rotation as the orbital angular momentum vector. The VEGA visible continuum data indicate an elongated shape for the Be star itself, due to the combined effects of rapid rotation, partial obscuration of the photosphere by the circumstellar disk, and flux from the bright inner disk.
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