论文标题
PTFO 8-8695B具有五年光学/红外监测观测值的行星假设的证据
Evidence for planetary hypothesis for PTFO 8-8695b with five-year optical/infrared monitoring observations
论文作者
论文摘要
PTFO 8-8695b（CVSO 30b）是一位年轻的行星候选人，其主机是$ \ sim $ 2.6 $ 2.6 Myr over T-Tauri Star，并且一直在讨论该系统的性质。为了揭露该系统的奥秘，我们在光学和红外频带上使用Higashi-Hiroshima天文台的Kanata望远镜同时观察了PTFO8-8695大约五年。通过我们的观察结果，我们发现据报道的褪色事件分为两个：更深但相移的“ DIP-A”和较浅但较浅但设备的“ DIP-B”。这些倾角在不同的时期消失，然后DIP-B重新出现。基于观察到的浸入深度的波长依赖性，尘埃团块和进攻行星可能分别是DIP-A和B的起源。在这里，我们建议该系统的“与尘埃云相关的进攻行星”。这种情况与报道的褪色事件深度变化，甚至与报道的结果变化是一致的，即使结果被认为是行星假设的负面证据，例如过去的rossiter-mclaughlin效应的过去未检测。如果这种情况是正确的，那么这是围绕前序列星的年轻（<3 Myr）行星的第三种情况。这一发现意味着可以在几名Myr中形成行星。
PTFO 8-8695b (CVSO 30b) is a young planet candidate whose host star is a $\sim$ 2.6 Myr-old T-Tauri star, and there have been continuous discussions about the nature of this system. To unveil the mystery of this system, we observed PTFO8-8695 for around five years at optical and infrared bands simultaneously using Kanata telescope at the Higashi-Hiroshima Observatory. Through our observations, we found that the reported fading event split into two: deeper but phase-shifted "dip-A" and shallower but equiphase "dip-B". These dips disappeared at different epochs, and then, dip-B reappeared. Based on the observed wavelength dependence of dip depths, a dust clump and a precessing planet are likely origins of dip-A and B, respectively. Here we propose "a precessing planet associated with a dust cloud" scenario for this system. This scenario is consistent with the reported change in the depth of fading events, and even with the reported results, which were thought to be negative evidence to the planetary hypothesis, such as the past non-detection of the Rossiter-McLaughlin effect. If this scenario is correct, this is the third case of a young (<3 Myr) planet around a pre-main sequence star. This finding implies that a planet can be formed within a few Myr.
