Kinematic signatures of a low-mass planet with a moderately inclined orbit in a protoplanetary disk

IF 2.2 4区 物理与天体物理 Q2 ASTRONOMY & ASTROPHYSICS Publications of the Astronomical Society of Japan Pub Date : 2023-09-14 DOI:10.1093/pasj/psad059
Kazuhiro D Kanagawa, Tomohiro Ono, Munetake Momose
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Abstract

Abstract A planet embedded in a protoplanetary disk produces a gap by disk–planet interaction. It also generates velocity perturbation of gas, which can also be observed as deviations from the Keplerian rotation in the channel map of molecular line emission, called kinematic planetary features. These observed signatures provide clues to determine the mass of the planet. We investigated the features induced by a planet with an inclined orbit through three-dimensional hydrodynamic simulations. We found that a smaller planet, with an inclination of ∼10○–20○, can produce kinematic features as prominent as those induced by a massive coplanar planet. Despite the kinematic features being similar, the gap is shallower and narrower compared with the case in which the kinematic features are formed by a coplanar planet. We also found that the kinematic features induced by an inclined planet were fainter for rarer CO isotopologues because the velocity perturbation is weaker at the position closer to the midplane, which was different in the case with a coplanar massive planet. This dependence on the isotopologues is distinguished if the planet has an inclined orbit. We discussed two observed kinematic features in the disk of HD 163296. We concluded that the kink observed at 220 au can be induced by an inclined planet, while the kink at 67 au is consistent to that induced by a coplanar planet.
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在原行星盘中有中等倾斜轨道的低质量行星的运动特征
嵌入原行星盘中的行星通过盘-行星相互作用产生间隙。它还会产生气体的速度扰动,这也可以在分子线发射的通道图中观察到与开普勒旋转的偏差,称为运动学行星特征。这些观测到的特征为确定行星的质量提供了线索。通过三维流体力学模拟,研究了倾斜轨道行星所引起的特征。我们发现,一个较小的行星,倾角为~ 10〇-20〇,可以产生与大质量共面行星引起的运动特征一样突出。尽管运动学特征相似,但与共面行星形成运动学特征的情况相比,间隙更浅,更窄。我们还发现,对于稀有的CO同位素物,倾斜行星引起的运动特征较弱,因为靠近中平面的位置的速度扰动较弱,这与共面大质量行星的情况不同。如果行星的轨道是倾斜的,这种对同位素的依赖就会被区分出来。我们讨论了HD 163296盘的两个观察到的运动学特征。我们得出结论,在220 au处观测到的扭结可以由倾斜行星引起,而在67 au处观测到的扭结与共面行星引起的扭结一致。
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来源期刊
Publications of the Astronomical Society of Japan
Publications of the Astronomical Society of Japan 地学天文-天文与天体物理
CiteScore
4.10
自引率
13.00%
发文量
98
审稿时长
4-8 weeks
期刊介绍: Publications of the Astronomical Society of Japan (PASJ) publishes the results of original research in all aspects of astronomy, astrophysics, and fields closely related to them.
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