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首页> 外文期刊>The Astrophysical journal >Detection Of A Hot Subdwarf Companion To The Be Star Fy Canis Majoris
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Detection Of A Hot Subdwarf Companion To The Be Star Fy Canis Majoris

机译：检测到一个热的矮人伴侣成为大明星犬大犬

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摘要

The rapid rotation of Be stars may be caused in some cases by past mass and angular momentum accretion in an interacting binary in which the mass donor is currently viewed as a small, hot subdwarf stripped of its outer envelope. Here we report on the spectroscopic detection of such a subdwarf in the Be binary system FY Canis Majoris from the analysis of data acquired by the IUE spacecraft and KPNO Coude Feed Telescope over the course of 16 and 21 yr, respectively. We present a double-lined spectroscopic orbit for the binary based on radial velocities from the IUE spectra and use the orbital solutions with a Doppler tomography algorithm to reconstruct the components' UV spectra. The subdwarf is hot (T_(eff) = 45 ± 5 kK) and has a mass of about 1.3 M_☉ and a radius of about 0.6 R_☉. It contributes about 4% as much flux as the Be star does in the FUV. We also present observations of the Ha and He λ661% emission features that are formed in the.circumstellar disk of the Be star. Orbital flux and velocity variations in the He I λ6678 profile indicate that much of the emission forms along the disk rim facing the hot subdwarf where the disk is probably heated by the incident radiation from the subdwarf. A study of the FUV infall shell lines discovered in the 1980s confirms their episodic presence but reveals that they tend to be found around both quadrature phases, unlike the pattern in Algol binaries. Phase-dependent variations in the UV N v doublet suggest the presence of a N-enhanced wind from the subdwarf and a possible shock-interaction region between the stars where the subdwarf's wind collides with the disk of the Be star.
机译：在某些情况下，Be星的快速旋转可能是由于相互作用的双星中过去的质量和角动量增加而引起的，在该相互作用的双星中，当前将质量给体看作是剥去了外壳的热小矮子。在这里，我们通过对IUE航天器和KPNO Coude馈电望远镜分别在16年和21年的过程中获得的数据进行分析，报告了Be双星系统FY Canis Majoris中这种亚矮的光谱检测。我们根据来自IUE光谱的径向速度为双星提供了双线光谱轨道，并将该轨道解与多普勒层析成像算法一起使用来重建组件的UV光谱。次矮体是热的（T_（eff）= 45±5 kK），质量约为1.3M_☉，半径约为0.6R_☉。它在FUV中的贡献约为Be星的4％。我们还介绍了在Be星的星际盘上形成的Ha和Heλ661％发射特征的观测结果。 He Iλ6678剖面中的轨道通量和速度变化表明，沿着面向热亚矮的圆盘边缘的许多发射形式，其中该盘可能被亚矮的入射辐射加热。一项对1980年代发现的FUV内陷壳线的研究证实了它们的偶发性存在，但揭示了它们倾向于在两个正交相附近找到，这与Algol双星模式不同。 UV N v doublet的相位相关变化表明，存在来自亚矮星的N增强风，以及恒星之间可能存在的冲击相互作用区域，其中亚矮星的风与Be恒星盘碰撞。

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