The yellow hypergiant HR 5171 A: Resolving a massive interacting binary in the common envelope phase
The yellow hypergiant HR 5171 A: Resolving a massive interacting binary in the common envelope phase
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黄色超巨星 HR 5171 A：在共同包络相中解析一个巨大的相互作用双星
DOI：
10.1051/0004-6361/201322421
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发表时间：
2014
影响因子：
6.5
通讯作者：
Chesneau O
中科院分区：
文献类型：
--
作者：
Chesneau O
只有少数恒星在快速穿过赫兹-罗素图时，被捕捉到了非常短暂而且往往是关键的阶段，我们启动了对大质量和不稳定的黄超巨星（YHG）直径的长期光学干涉测量监测，目的是探测其半径的长期演变和可能的赝超巨星的短期形成。方法我们用AMBER/VLTI观测了HR 5171 A。我们还研究了档案测光数据的视觉和近红外跨越60多年，以及稀疏的光谱data.ResultsHR 5171 A表现出复杂的外观。我们的AMBER数据揭示了一颗令人惊讶的大星星，其YHGR半径为1315 ± 260 R（或~6.1 Au），距离为3.6 ± 0.5 kpc。该源被一个扩展的星云包围，这些数据也显示了该系统亮度分布的不对称性，我们将其归因于一颗新发现的位于主星星星前面的伴星星星。伴星的特征也在目视测光中被探测到，它的轨道周期为Porb = 1304 ± 6 d。用NIGHTFALL程序模拟光变曲线提供了明确的证据，证明该系统是一个接触或可能过接触的食双星。HR 5171 A的低质量伴星非常接近其密风中的主星星星。缺乏对初级的倾斜度和vsini的严格约束，这使我们无法精确地确定其对质量损失现象的影响，但该系统可能正在经历风罗切叶溢出。根据转移到恒星包层的角动量的大小，HR 5171 A可能会成为一颗快速旋转的B[e]/明亮的蓝色变星/沃尔夫-拉叶星星。无论如何，HR 5171 A强调了双星对于解释不稳定的YHG和大质量星星演化的可能重要性。
ContextOnly a few stars are caught in the very brief and often crucial stages when they quickly traverse the Hertzsprung-Russell diagram, and none has yet been spatially resolved in the mass transfer phase.AimsWe initiated long-term optical interferometry monitoring of the diameters of massive and unstable yellow hypergiants (YHG) with the goal of detecting both the long-term evolution of their radius and shorter term formation of a possible pseudo-photosphere related to proposed large mass-loss events.MethodsWe observed HR 5171 A with AMBER/VLTI. We also examined archival photometric data in the visual and near-IR spanning more than 60 years, as well as sparse spectroscopic data.ResultsHR 5171 A exhibits a complex appearance. Our AMBER data reveal a surprisingly large star for a YHGR∗= 1315 ± 260R⊙(or ~6.1 AU) at the distance of 3.6 ± 0.5 kpc. The source is surrounded by an extended nebulosity, and these data also show a large level of asymmetry in the brightness distribution of the system, which we attribute to a newly discovered companion star located in front of the primary star. The companion’s signature is also detected in the visual photometry, which indicates an orbital period ofPorb= 1304 ± 6 d. Modeling the light curve with the NIGHTFALL program provides clear evidence that the system is a contact or possibly over-contact eclipsing binary. A total current system mass of 39+40-22M⊙and a high mass ratioq≥ 10 is inferred for the system.ConclusionsThe low-mass companion of HR 5171 A is very close to the primary star that is embedded within its dense wind. Tight constraints on the inclination andvsiniof the primary are lacking, which prevents us from determining its influence precisely on the mass-loss phenomenon, but the system is probably experiencing a wind Roche-Lobe overflow. Depending on the amount of angular momentum that can be transferred to the stellar envelope, HR 5171 A may become a fast-rotating B[e]/luminous blue variable/Wolf-Rayet star. In any case, HR 5171 A highlights the possible importance of binaries for interpreting the unstable YHGs and for massive star evolution in general.
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