Protoplanetary disc evolution affected by star-disc interactions in young stellar clusters
Protoplanetary disc evolution affected by star-disc interactions in young stellar clusters
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DOI：
10.1093/mnras/stu679
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发表时间：
2014-04
影响因子：
4.8
通讯作者：
G. Rosotti;J. Dale;M. D. Ovelar;D. Hubber;J. Kruijssen;B. Ercolano;S. Walch
中科院分区：
文献类型：
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作者：
G. Rosotti;J. Dale;M. D. Ovelar;D. Hubber;J. Kruijssen;B. Ercolano;S. Walch
大多数恒星形成于一个集群环境中。因此，重要的是评估这种环境如何影响年轻恒星周围原行星盘的演化。反过来，这会影响它们产生行星并最终产生生命的能力。我们在这里首次提出了3D SPH/N体模拟，包括其纳塔尔恒星周围的光盘的流体动力学演化，以及恒星本身的动力学。这些圆盘是粘性演化的，将质量吸积到中心的星星上并扩散。我们发现穿透性的遭遇对椎间盘的破坏性很大，就像以前的研究一样，尽管这种遭遇的频率很低。然而，我们也发现，遇到的影响更强烈的光盘半径比其他光盘的属性，如光盘质量。圆盘的大小是由粘性扩散和碰撞的破坏性影响之间的竞争决定的。随着光盘的传播，相遇变得越来越重要。在迅速蔓延的政权遇到简单地截断光盘，剥离外部部分。在相反的制度，我们发现，许多遥远的遭遇的影响是能够限制盘的大小。最后，我们预测，从我们的模拟，光盘的大小是有限的恒星密度超过2 - 3 - 10 - 3 PC 2的遭遇。
Most stars form in a clustered environment. Therefore, it is important to assess how this environment influences the evolution of protoplanetary discs around young stars. In turn, this affects their ability to produce planets and ultimately life. We present here for the first time 3D SPH/N-body simulations that include both the hydrodynamical evolution of the discs around their natal stars, as well as the dynamics of the stars themselves. The discs are viscously evolving, accreting mass onto the central star and spreading. We find penetrating encounters to be very destructive for the discs as in previous studies, although the frequency of such encounters is low. We also find, however, that encounter influence the disc radii more strongly than other disc properties such as the disc mass. The disc sizes are set by the competition between viscous spreading and the disruptive effect of encounters. As discs spread, encounters become more and more important. In the regime of rapid spreading encounters simply truncate the discs, stripping the outer portions. In the opposite regime, we find that the effect of many distant encounters is able to limit the disc size. Finally, we predict from our simulations that disc sizes are limited by encounters at stellar densities exceeding 2 3 10 3 pc 2 .