论文标题
恒星形成区域中的原球盘半径和圆盘质量的演变
The evolution of protoplanetary disc radii and disc masses in star-forming regions
论文作者
论文摘要
原球盘对于理解行星的形成和发展至关重要，但是这些物体受宿主恒星的出生环境的变化。特别是，来自大型恒星的光电离辐射已被证明是破坏原球盘的有效药物。外部光蒸发导致光盘半径的内向演变，而圆盘的内部粘性演变会导致半径向外进化。我们将恒星形成区域的N体模拟与圆盘进化的后处理分析，以确定年轻恒星形成区域中原星盘的半径和质量分布如何进化。为了与观察一致，我们发现最初的圆盘半径必须为100AU，即使这些圆盘很容易被大型恒星的光蒸发破坏。此外，猎户座星云群中观察到的圆盘半径分布与中等初始恒星密度（100m $ _ \ odot $ pc $^{ - 3} $）更加一致，其动力学模型认为，ONC的内在密度更高。此外，如果其圆盘受外部光蒸发，我们无法再现狼疮恒星形成区域中观察到的圆盘半径分布。由于有据可查的不确定性在确定前序列序列（圆盘托管）恒星的年龄时，无法进行更详细的比较。
Protoplanetary discs are crucial to understanding how planets form and evolve, but these objects are subject to the vagaries of the birth environments of their host stars. In particular, photoionising radiation from massive stars has been shown to be an effective agent in disrupting protoplanetary discs. External photoevaporation leads to the inward evolution of the radii of discs, whereas the internal viscous evolution of the disc causes the radii to evolve outwards. We couple N-body simulations of star-forming regions with a post-processing analysis of disc evolution to determine how the radius and mass distributions of protoplanetary discs evolve in young star-forming regions. To be consistent with observations, we find that the initial disc radii must be of order 100au, even though these discs are readily destroyed by photoevaporation from massive stars. Furthermore, the observed disc radii distribution in the Orion Nebula Cluster is more consistent with moderate initial stellar densities (100M$_\odot$ pc$^{-3}$), in tension with dynamical models that posit much higher inital densities for the ONC. Furthermore, we cannot reproduce the observed disc radius distribution in the Lupus star-forming region if its discs are subject to external photoevaporation. A more detailed comparison is not possible due to the well-documented uncertainties in determining the ages of pre-main sequence (disc-hosting) stars.
