Photoevaporation of protoplanetary discs II: evolutionary models and observable properties
Photoevaporation of protoplanetary discs II: evolutionary models and observable properties
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DOI：
10.1111/j.1365-2966.2006.10294.x
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发表时间：
2006-03
期刊：
影响因子：
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通讯作者：
R.D.Alexander;C.J.Clarke;J.E.Pringle
中科院分区：
文献类型：
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作者：
R.D.Alexander;C.J.Clarke;J.E.Pringle
我们提出了一个新的原行星盘演化模型。这个模型结合了粘性演化和圆盘的光蒸发，其方式类似于Clarke，Gendrin & Sotomayor（2001）。然而，在一篇配套论文（亚历山大、克拉克和普林格尔2006 a）中，我们已经表明，在后期，此类模型必须考虑直接入射到内盘边缘的恒星辐射的影响，在这里我们对该过程的观测影响进行了建模。我们发现，整个光盘是分散在一个时间尺度上的顺序10 - 5年后，光盘寿命的几个百万年，与金牛座T（TT）恒星的观测一致。我们使用一个简单的处方来模拟不断发展的光盘的光谱能量分布，并证明该模型是一致的观测数据在很宽的波长范围。我们还注意到，该模型预测一个短的“内孔”阶段的所有TT光盘的演变，并在中红外和毫米波长的未来观测作出预测。
We present a new model for protoplanetary disc evolution. This model combines viscous evolution with photoevaporationof the disc, in a manner similar to Clarke, Gendrin & Sotomayor (2001). However in a companion paper (Alexander, Clarke & Pringle 2006a) we have shown that at late times such models must consider the e ff ect of stellar radiation directly incident on the inner disc edge, and here we model the observational implications of this process. We find that the entire disc is dispersed on a time-scale of order 10 5 yr after a disc lifetime of a few Myr, consistent with observations of T Tauri (TT) stars. We use a simple prescription to model the spectral energy distribution of the evolving disc, and demonstrate that the model is consistent with observational data across a wide range of wavelengths. We note also that the model predicts a short “inner hole” phase in the evolution of all TT discs, and make predictions for future observations at mid-infrared and millimetre wavelengths.