On the structure and mass delivery towards circumplanetary discs
On the structure and mass delivery towards circumplanetary discs
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关于环行星盘的结构和质量传递
DOI：
10.1051/0004-6361/202037556
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发表时间：
2020
影响因子：
6.5
通讯作者：
M. Lambrechts
中科院分区：
文献类型：
--
作者：
Matthäus Schulik;A. Johansen;B. Bitsch;E. Lega;M. Lambrechts
围绕年轻气态巨行星形成的环行星盘（CPD）被认为是月球形成的场所，也是为气态巨星生长提供营养的中间气体储层。人们对此类 CPD 的物理特性如何受到行星质量和整体不透明度的影响相对知之甚少。为了澄清这一点，我们使用了具有网格结构的全球辐射流体动力学代码 FARGOCA，该代码可以充分解析形成 CPD 的行星引力势。然后，我们研究了作为行星质量、不透明度和潜在深度的函数出现的气流和密度-温度结构。我们的结果表明，木星质量行星在低不透明度下形成了有趣的结构，我们随后对其进行了详细分析。我们的木星质量原行星使用比星际介质尘埃低 100 倍的不透明度，具有足够冷的包层以形成 CPD，以及将 CPD 和出现的星周盘分开的自由落体区域。有趣的是，这个自由落体区域似乎是外壳材料超音速侵蚀的结果，而不是在低不透明度下预期的静态结构形成。我们的分析表明，行星旋臂似乎构成了一个重要的压力屏障，需要通过辐射冷却来克服，以便气体能够积聚到 CPD 上。 CPD 内部的循环接近开普勒式，并因 CPD 旋臂的存在而改变。当我们增加行星势深度时，情况也是如此，这反过来又增加了行星光度，抑制了自由落体区域的形成，并使包层的旋转速度降低了 10%。对于高不透明度，我们从文献中恢复结果，找到了几乎没有特征的热信封。通过这项工作，我们首次在 3D 辐射流体动力学环境中模拟和分析了原行星与其母盘的完整分离过程。
Circumplanetary discs (CPDs) that form around young gas giants are thought to be the sites of moon formation as well as an intermediate reservoir of gas that feeds the growth of the gas giant. How the physical properties of such CPDs are affected by the planetary mass and the overall opacity is relatively poorly understood. In order to clarify this, we used the global radiation hydrodynamics code FARGOCA with a grid structure that allows sufficient resolution of the planetary gravitational potential for a CPD to form. We then studied the gas flows and density–temperature structures that emerge as a function of planet mass, opacity, and potential depth. Our results indicate interesting structure formation for Jupiter-mass planets at low opacities, which we subsequently analysed in detail. Using an opacity level that is 100 times lower than that of the dust of the interstellar medium, our Jupiter-mass protoplanet features an envelope that is sufficiently cold for a CPD to form, and a free-fall region separating the CPD and the circumstellar disc that emerges. Interestingly, this free-fall region appears to be the result of supersonic erosion of outer envelope material, as opposed to the static structure formation that one would expect at low opacities. Our analysis reveals that the planetary spiral arms seem to pose a significant pressure barrier that needs to be overcome through radiative cooling in order for gas to be accreted onto the CPD. The circulation inside the CPD is near-Keplerian and is modified by the presence of CPD spiral arms. The same is true when we increase the planetary potential depth, which in turn increases the planetary luminosity, quenches the formation of a free-fall region, and decreases the rotation speed of the envelope by 10%. For high opacities, we recover results from the literature, finding an almost featureless hot envelope. With this work, we demonstrate the first simulation and analysis of a complete detachment process of a protoplanet from its parent disc in a 3D radiation hydrodynamics setting.
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DOI：
10.1088/0004-637x/807/1/2
发表时间：
2015-05
期刊：
The Astrophysical Journal
影响因子：
--
作者：
L. Cleeves;E. Bergin;T. J. H. U. O. Michigan;U. Exeter
通讯作者：
L. Cleeves;E. Bergin;T. J. H. U. O. Michigan;U. Exeter
DOI：
10.1111/j.1365-2966.2008.14184.x
发表时间：
2008-11
影响因子：
4.8
作者：
Ben A. Ayliffe;M. Bate
通讯作者：
Ben A. Ayliffe;M. Bate
DOI：
10.3847/2041-8213/aaf742
发表时间：
2018-12
期刊：
The Astrophysical Journal Letters
影响因子：
--
作者：
C. Dullemond;T. Birnstiel;Jane Huang;N. Kurtovic;S. Andrews;V. Guzm'an;L. P'erez;A. Isella;Zhaohuan Zhu;M. Benisty;D. Wilner;X. Bai;J. Carpenter;Shangjia Zhang;L. Ricci
通讯作者：
C. Dullemond;T. Birnstiel;Jane Huang;N. Kurtovic;S. Andrews;V. Guzm'an;L. P'erez;A. Isella;Zhaohuan Zhu;M. Benisty;D. Wilner;X. Bai;J. Carpenter;Shangjia Zhang;L. Ricci
DOI：
10.3847/2041-8213/ab2a12
发表时间：
2019-06
期刊：
The Astrophysical Journal Letters
影响因子：
--
作者：
A. Isella;M. Benisty;R. Teague;J. Bae;M. Keppler;S. Facchini;L. P'erez
通讯作者：
A. Isella;M. Benisty;R. Teague;J. Bae;M. Keppler;S. Facchini;L. P'erez