Simultaneous Spectral Energy Distribution and Near-infrared Interferometry Modeling of HD 142666
Simultaneous Spectral Energy Distribution and Near-infrared Interferometry Modeling of HD 142666
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DOI：
10.3847/1538-4357/aade51
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发表时间：
2018-08
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影响因子：
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通讯作者：
C. Davies;S. Kraus;T. Harries;A. Kreplin;J. Monnier;A. Labdon;B. Kloppenborg;D. Acreman;F. Baron
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文献类型：
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作者：
C. Davies;S. Kraus;T. Harries;A. Kreplin;J. Monnier;A. Labdon;B. Kloppenborg;D. Acreman;F. Baron
我们提出了赫比格Ae星HD 142666的综合模型，旨在同时解释它的光谱能量分布和近红外干涉测量。我们新的亚毫角秒分辨率查拉(经典和攀登)干涉观测，补充了来自VLTI/Pionier和Keck干涉仪的较短的基线数据，使用了中心对称几何模型和轴对称辐射传输代码。Chara的330米基线使我们能够对观察几何图形施加强烈的约束，显示出一个与面对面成58°倾斜的圆盘，主轴位置角度为160°。施加垂直静力平衡的圆盘模型对SED的拟合很差。考虑到可能由与磁致旋转不稳定性相关的湍流引起的盘片尺度高度膨胀，以及在盘片边缘中的颗粒生长到≳1μm尺寸的模型，需要同时再现SED和测量的能见度分布。然而，我们最好的模型符合SED的能见度残差表明存在无法解释的近红外发射，特别是沿着视盘短轴，而闭合相残差表明发射区域更加中心对称。此外，我们推断的58°椎间盘倾斜度与HD 142666表现出的UX ORI型变异性的基于磁盘的起源不一致。在我们的模型中没有考虑到的额外的复杂性，显然存在于近红外发射区。我们认为，圆盘可能倾向于更多的边缘方向和/或光学厚度的流出成分也对近红外星际流量有贡献。
We present comprehensive models of the Herbig Ae star, HD 142666, which aim to simultaneously explain its spectral energy distribution (SED) and near-infrared (NIR) interferometry. Our new submilliarcsecond resolution CHARA (CLASSIC and CLIMB) interferometric observations, supplemented with archival shorter baseline data from VLTI/PIONIER and the Keck Interferometer, are modeled using centrosymmetric geometric models and an axisymmetric radiative transfer code. CHARA’s 330 m baselines enable us to place strong constraints on the viewing geometry, revealing a disk inclined at 58° from face-on with a 160° major axis position angle. Disk models imposing vertical hydrostatic equilibrium provide poor fits to the SED. Models accounting for disk scale height inflation, possibly induced by turbulence associated with magnetorotational instabilities, and invoking grain growth to ≳1 μm size in the disk rim are required to simultaneously reproduce the SED and measured visibility profile. However, visibility residuals for our best model fits to the SED indicate the presence of unexplained NIR emission, particularly along the apparent disk minor axis, while closure phase residuals indicate a more centrosymmetric emitting region. In addition, our inferred 58° disk inclination is inconsistent with a disk-based origin for the UX Ori-type variability exhibited by HD 142666. Additional complexity, unaccounted for in our models, is clearly present in the NIR-emitting region. We propose that the disk is likely inclined toward a more edge-on orientation and/or an optically thick outflow component also contributes to the NIR circumstellar flux.