arXiv 2010.096712020-10astro-ph.EPastro-ph.GAastro-ph.IM

自由浮动行星和矮行星的质量

Masses for Free-Floating Planets and Dwarf Planets

Andrew Gould, Weicheng Zang, Shude Mao, Subo Dong

备注：: RAA, in press
DOI：: 10.1088/1674-4527/21/6/133

摘要：

自由浮动行星（FFP）的质量和距离函数将为行星系的形成和演化提供重要的见解，包括圆盘和凸起之间的任何系统差异。我们表明，唯一的方法来测量的质量和距离的个别FFP在一个广泛的距离范围是同时观察他们从两个观测站分开的$D\sim {\cal O}(0.01\,AU)$（测量他们的微透镜视差$π_{\rm E}$）和集中在有限源点透镜（FSPL）事件（产生爱因斯坦半径$θ_{\rm E}$）。通过将现有的KMTNet 3望远镜天文台与L2的0.3米$4\,{\rm deg}^2$望远镜相结合，可以在四年内进行130次这样的测量，对于凸起的FFP，可以降低到大约$M\sim 6\,M_\oplus$，对于盘状FFP，可以降低到$M\sim 0.7\,M_\oplus$。同样的实验将返回许多束缚行星系的质量和距离。一个更雄心勃勃的实验，有两个0.5米的卫星（一个在L2，另一个更接近地球）和类似的相机布局，但在红外线，可以测量质量和距离的月球质量物体，从而探测（和区分）真正的月球下的FFP和月球下的“矮行星”在exo-Kuiper带和exo-奥尔特云。

英文摘要：

The mass and distance functions of free-floating planets (FFPs) would give major insights into the formation and evolution of planetary systems, including any systematic differences between those in the disk and bulge. We show that the only way to measure the mass and distance of individual FFPs over a broad range of distances is to observe them simultaneously from two observatories separated by $D\sim {\cal O}(0.01\,AU)$ (to measure their microlens parallax $π_{\rm E}$) and to focus on the finite-source point-lens (FSPL) events (which yield the Einstein radius $θ_{\rm E}$). By combining the existing KMTNet 3-telescope observatory with a 0.3m $4\,{\rm deg}^2$ telescope at L2, of order 130 such measurements could be made over four years, down to about $M\sim 6\,M_\oplus$ for bulge FFPs and $M\sim 0.7\,M_\oplus$ for disk FFPs. The same experiment would return masses and distances for many bound planetary systems. A more ambitious experiment, with two 0.5m satellites (one at L2 and the other nearer Earth) and similar camera layout but in the infrared, could measure masses and distances of sub-Moon mass objects, and thereby probe (and distinguish between) genuine sub-Moon FFPs and sub-Moon ``dwarf planets'' in exo-Kuiper Belts and exo-Oort Clouds.

机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。

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