arXiv 2408.096142024-08astro-ph.EPastro-ph.SR

发现HD 73344中一颗与内行星系统错位的木星类似天体

Discovery of a Jupiter Analog Misaligned to the Inner Planetary System in HD 73344

Jingwen Zhang, Lauren M. Weiss, Daniel Huber, Jerry W. Xuan, Michael Bottom, Benjamin J. Fulton, Howard Isaacson, Mason G. MacDougall, Nicholas Saunders

备注：: 21 pages, 12 figures, accepted by AJ. arXiv admin note: text overlap with arXiv:2407.21377

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AI总结：

本研究利用27年视向速度、TESS及Hipparcos-Gaia数据发现HD 73344 d，并证明其与内行星系统显著错位，揭示了行星散射或原行星盘扭曲的演化线索。

摘要：

我们基于27年的视向速度观测，报告发现一颗类木行星HD 73344 d，其质量为$m_{d}=2.55^{+0.56}_{-0.46}\\ \mathrm{M_{J}}$，半长轴为$a_{d}=6.70^{+0.25}_{-0.26}$ AU，偏心率为$e_{d}=0.18^{+0.14}_{-0.12}$。HD 73344还拥有一个致密的内行星系统，包括一颗凌星亚海王星HD 73344 b（周期$P_{b}=15.61\\ \mathrm{days}$，半径$r_{b}=2.88^{+0.08}_{-0.07}\\ \mathrm{R_{\oplus}}$）和一颗不凌星的土星质量行星（周期$P_{c}=65.936\\ \mathrm{days}$，$m_{c}\sin{i_c}=0.36^{+0.02}_{-0.02}\\ \mathrm{M_{J}}$）。通过分析TESS光变曲线，我们确定恒星自转周期为$9.03\pm{1.3}$天。将其与恒星光谱测得的$v\sin{i_*}$相结合，我们得到恒星倾角为$63.6^{+17.4}_{-16.5}\\ \rm{deg}$。此外，通过结合视向速度和Hipparcos-Gaia天体测量加速度，我们表征了外侧巨行星的三维轨道，并将其相对于最内侧凌星行星的相互倾角约束为$46 <ΔI_{bd}< 134\\ \rm{deg}\\ (1σ)$和$20 <ΔI_{bd}< 160\\ \rm{deg}\\ (2σ)$，强烈排除共面结构。我们的解析计算和N体模拟表明，两颗内行星彼此强耦合，并围绕巨行星的轨道轴共同发生交点进动。在交点进动期间，内行星的轨道倾角随时间振荡，因此相对于恒星自转轴变得错位。此类系统的形成表明其曾经历行星-行星散射，或原行星盘内、外成分之间存在错位。即将发布的Gaia DR4将发现更多类似HD 73344的系统，并使在统计层面研究兼具内、外行星系统的系外行星系统的平坦度成为可能。

英文摘要：

We present the discovery of a Jupiter-like planet, HD 73344 d ($m_{d}=2.55^{+0.56}_{-0.46}\ \mathrm{M_{J}}$, $a_{d}=6.70^{+0.25}_{-0.26}$ AU, $e_{d}=0.18^{+0.14}_{-0.12}$) based on 27-year radial velocity observations. HD 73344 also hosts a compact inner planetary system, including a transiting sub-Neptune HD 73344 b ($P_{b}=15.61\ \mathrm{days}$, $r_{b}=2.88^{+0.08}_{-0.07}\ \mathrm{R_{\oplus}}$) and a non-transiting Saturn-mass planet ($P_{c}=65.936\ \mathrm{days}$, $m_{c}\sin{i_c}=0.36^{+0.02}_{-0.02}\ \mathrm{M_{J}}$). By analyzing TESS light curves, we identified a stellar rotation period of $9.03\pm{1.3}$ days. Combining this with $v\sin{i_*}$ measurements from stellar spectra, we derived a stellar inclination of $63.6^{+17.4}_{-16.5}\ \rm{deg} $. Furthermore, by combining radial velocities and Hipparcos-Gaia astrometric acceleration, we characterized the three-dimensional orbit of the outer giant planet and constrained its mutual inclination relative to the innermost transiting planet to be $46 <ΔI_{bd}< 134\ \rm{deg}\ (1σ)$ and $20 <ΔI_{bd}< 160\ \rm{deg}\ (2σ)$, strongly disfavoring coplanar architectures. Our analytical calculations and N-body simulation reveal that the two inner planets are strongly coupled with each other and undergo nodal precession together around the orbital axis of the giant planet. During nodal precession, the orbital inclination of inner planets oscillate with time and therefore become misaligned relative to the stellar spin axis. The formation of such systems suggests a history of planet-planet scattering or misalignment between the inner and outer components of protoplanetary disks. The upcoming release of Gaia DR4 will uncover more systems similar to HD 73344 and enable the study of the flatness of exoplanet systems with a mixture of inner and outer planetary systems on a statistical level.

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