The effects of disc self-gravity and radiative cooling on the formation of gaps and spirals by young planets
The effects of disc self-gravity and radiative cooling on the formation of gaps and spirals by young planets
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DOI：
10.1093/mnras/staa404
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发表时间：
2019-11
影响因子：
4.8
通讯作者：
Shangjia Zhang;Zhaohuan Zhu
中科院分区：
文献类型：
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作者：
Shangjia Zhang;Zhaohuan Zhu
我们进行了二维流体动力学模拟，以研究圆盘自重力和辐射冷却对间隙和螺旋形成的影响。 (1) 考虑到圆盘的自重力，我们发现更大质量的圆盘具有更强、更紧密缠绕的螺旋和更深的间隙。正如线性理论所预期的那样，更深的间隙是由于在更大质量的圆盘中激发的波的角动量通量（AMF）更大。如果圆盘质量不是特别大（Q ≳ 2），则次级间隙的位置不会改变。 (2) 当包括辐射冷却时，随着圆盘冷却时间尺度的增加，受激螺旋变得单调地更加开放（缠绕不那么紧密）。另一方面，当冷却时间从很小的值增加到~1/Ω时，螺旋的振幅和强度下降，但当冷却时间继续增加时，振幅又开始增加。这表明辐射耗散对于 Tcool ∼ 1 的波来说变得很重要。因此，当冷却时间变为 ∼1/Ω 时，感应的初级间隙更窄，次级间隙变得明显更浅。当存在二次间隙时，其位置从快冷箱向慢冷箱移动到内盘。间隙特性对冷却时间尺度的依赖性（例如在 AS 209 中）提供了一种限制光盘光学深度以及光盘表面密度的新方法。
We have carried out 2D hydrodynamical simulations to study the effects of disc self-gravity and radiative cooling on the formation of gaps and spirals. (1) With disc self-gravity included, we find stronger, more tightly wound spirals and deeper gaps in more massive discs. The deeper gaps are due to the larger Angular Momentum Flux (AMF) of the waves excited in more massive discs, as expected from the linear theory. The position of the secondary gap does not change, provided that the disc is not extremely massive (Q ≳ 2). (2) With radiative cooling included, the excited spirals become monotonically more open (less tightly wound) as the disc’s cooling time-scale increases. On the other hand, the amplitude and strength of the spirals decrease when the cooling time increases from a small value to ∼1/Ω, but then the amplitude starts to increase again when the cooling time continues to increase. This indicates that radiative dissipation becomes important for waves with Tcool ∼ 1. Consequently, the induced primary gap is narrower and the secondary gap becomes significantly shallower when the cooling time becomes ∼1/Ω. When the secondary gap is present, the position of it moves to the inner disc from the fast cooling cases to the slow cooling cases. The dependence of gap properties on the cooling time-scale (e.g. in AS 209) provides a new way to constrain the disc optical depth and thus disc surface density.