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arXiv 1906.01416astro-ph.EP
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形成中的行星和它们的环行星系III的可观测性。--偏振散射光

Observability of Forming Planets and their Circumplanetary Disks III. -- Polarized Scattered Light

J. Szulágyi, A. Garufi

备注：
Accepted at MNRAS
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摘要：

越来越多的星周盘的高分辨率偏振散射光图像。新生的巨行星行星被它们自己的环绕行星的圆盘所包围，这些圆盘可能会散射和反射行星和恒星的光。在这里，我们调查我们是否可以用同样的技术检测环行星盘，我们可以从这样的检测中学到什么。在这里，我们为SPHERE和GPI等仪器创建了1.245微米（J波段）的散射光模拟观测，用于各种行星质量（0.3，1.0，5.0，10.0 $\rm{M_{Jup}}$），圆盘倾角（90，60，30，0度）和行星位置角（0，45，90度）。我们发现，如果行星是大质量的（$\geq 5 \rm{M_{Jup}}$），并且系统几乎是面对面的（$\leq 30^\circ$），那么在距离恒星50天文单位处检测到环行星盘是非常有利的。在这些情况下，环行星盘表面的吸积激波阵面足够强和明亮，有助于子盘的可见性。它的探测受到邻近的拱星盘的阻碍，该盘也提供了强大的偏振通量。然而，$PI$和$Q_ϕ$地图之间的比较是一个可行的工具，可以精确定位环行星盘在拱星盘内的存在，因为这两个盘在这些图像上的表现不同。

英文摘要：

There are growing amount of very high-resolution polarized scattered light images of circumstellar disks. Nascent giant planets planets are surrounded by their own circumplanetary disks which may scatter and polarize both the planetary and stellar light. Here we investigate whether we could detect circumplanetary disks with the same technique and what can we learn from such detections. Here we created scattered light mock observations at 1.245 microns (J band) for instruments like SPHERE and GPI, for various planetary masses (0.3, 1.0, 5.0, 10.0 $\rm{M_{Jup}}$), disk inclinations (90, 60, 30, 0 degrees) and planet position angles (0, 45, 90 degrees). We found that the detection of a circumplanetary disk at 50AU from the star is significantly favored if the planet is massive ($\geq 5 \rm{M_{Jup}}$) and the system is nearly face-on ($\leq 30^\circ$). In these cases the accretion shock front on the surface of the circumplanetary disks are strong and bright enough to help the visibility of this subdisk. Its detection is hindered by the neighboring circumstellar disk that also provides a strong polarized flux. However, the comparison between the $PI$ and the $Q_ϕ$ maps is a viable tool to pinpoint the presence of the circumplanetary disk within the circumstellar disk, as the two disks are behaving differently on those images.

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