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首页> 外文期刊>The Astrophysical journal >OBSERVATIONS OF T TAURI DISKS AT SUB-AU RADII: IMPLICATIONS FOR MAGNETOSPHERIC ACCRETION AND PLANET FORMATION
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OBSERVATIONS OF T TAURI DISKS AT SUB-AU RADII: IMPLICATIONS FOR MAGNETOSPHERIC ACCRETION AND PLANET FORMATION

机译：SUB-AU半径T TAURI盘的观测：对磁球吸积和行星形成的影响

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摘要

We determine inner disk sizes and temperatures for four solar-type (1-2 solar mass) classical T Tauri stars, AS 207A, V2508 Oph, AS 205A, and PX Vul, using 2.2 μm observations from the Keck Interferometer. Nearly contemporaneous near-IR adaptive optics imaging photometry, optical photometry, and high-dispersion optical spectroscopy are used to distinguish contributions from the inner disks and central stars in the interferometric observations. In addition, the spectroscopic and photometric data provide estimates of stellar properties, mass accretion rates, and disk corotation radii. We model our interferometric and photometric data in the context of geometrically flat accretion disk models with inner holes, and flared disks with puffed-up inner walls. Models incorporating puifed-up inner disk walls generally provide better fits to the data, similar to previous results for higher mass Herbig Ae stars. Our measured inner disk sizes are larger than disk truncation radii predicted by magnetospheric accretion models, with larger discrepancies for sources with higher mass accretion rates. We suggest that our measured sizes correspond to dust sublimation radii, and that optically thin gaseous material may extend farther inward to the magnetospheric truncation radii. Finally, our inner disk measurements constrain the location of terrestrial planet formation as well as potential mechanisms for halting giant planet migration.
机译：我们使用来自Keck干涉仪的2.2μm观测值，确定了四个太阳型（1-2个太阳质量）经典T Tauri星，AS 207A，V2508 Oph，AS 205A和PX Vul的内盘大小和温度。几乎同时使用的近红外自适应光学成像光度法，光学光度法和高色散光谱法被用于区分干涉观测中来自内盘和中心恒星的贡献。此外，光谱和光度学数据还提供了恒星特性，吸积率和圆盘旋转半径的估计值。我们在具有内孔的几何平坦吸积盘模型和具有膨化内壁的扩口盘的背景下对干涉和光度学数据进行建模。结合有inner起的内盘壁的模型通常可以更好地拟合数据，类似于先前对质量较高的Herbig Ae星的结果。我们测得的内部磁盘大小大于磁层吸积模型预测的磁盘截断半径，对于质量吸积率较高的源，其差异更大。我们建议测得的尺寸对应于粉尘升华半径，而光学上稀薄的气态物质可能会向内延伸至磁层截断半径。最后，我们的内盘测量值限制了地球行星形成的位置以及阻止巨型行星迁移的潜在机制。

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