Probing the Inner Disk Emission of the Herbig Ae Stars HD 163296 and HD 190073
Probing the Inner Disk Emission of the Herbig Ae Stars HD 163296 and HD 190073
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DOI：
10.3847/1538-4357/aaef2c
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发表时间：
2018-11
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通讯作者：
B. Setterholm;J. Monnier;C. Davies;A. Kreplin;S. Kraus;F. Baron;A. Aarnio;J. Berger;N. Calvet-N.-Ca
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作者：
B. Setterholm;J. Monnier;C. Davies;A. Kreplin;S. Kraus;F. Baron;A. Aarnio;J. Berger;N. Calvet-N.-Ca
围绕赫比格Ae恒星的原行星盘内部几个天文单位内发生的物理过程对于设置外部行星形成盘演化的环境至关重要，并对吸积和行星迁移过程施加关键限制。我们提出了最完整的高角分辨率的H-和K-波段观测的恒星HD 163296和HD 190073，包括30个以前未发表的夜晚的观测前者和45个夜晚的后者与CHARA长基线干涉仪，除了档案VLTI数据公布的样本。我们证实了以前的观察表明，显着的近红外发射起源于假定的尘埃蒸发前的HD 163296，并表明这是HD 190073的情况。HD 163296和HD 190073的H和K波段大小相同，分别在（3 ± 3）%和（6 ± 10）%范围内。这两个磁盘的径向表面亮度轮廓是显着的高斯型，很少或根本没有迹象表明，预期的灰尘蒸发锋的尖锐边缘。结合光谱能量分布分析，我们在H和K波段对恒星通量分量的直接测量表明，HD 190073比以前认为的要年轻得多（<400 kyr），质量也更大（25.6 M），这主要是由于新的盖亚距离（891 pc）。
The physical processes occurring within the inner few astronomical units of protoplanetary disks surrounding Herbig Ae stars are crucial to setting the environment in which the outer planet-forming disk evolves and put critical constraints on the processes of accretion and planet migration. We present the most complete published sample of high angular resolution H- and K-band observations of the stars HD 163296 and HD 190073, including 30 previously unpublished nights of observations of the former and 45 nights of the latter with the CHARA long-baseline interferometer, in addition to archival VLTI data. We confirm previous observations suggesting that significant near-infrared emission originates within the putative dust evaporation front of HD 163296 and show that this is the case for HD 190073 as well. The H- and K-band sizes are the same within (3 ± 3)% for HD 163296 and within (6 ± 10)% for HD 190073. The radial surface brightness profiles for both disks are remarkably Gaussian-like with little or no sign of the sharp edge expected for a dust evaporation front. Coupled with spectral energy distribution analysis, our direct measurements of the stellar flux component at the H and K bands suggest that HD 190073 is much younger (<400 kyr) and more massive (∼5.6 M⊙) than previously thought, mainly as a consequence of the new Gaia distance (891 pc).