论文标题
$π$ mensae系统中行星之间的显着相互倾向
A significant mutual inclination between the planets within the $π$ Mensae system
论文作者
论文摘要
测量多行星外系统的几何形状可以洞悉其动力学历史和行星形成过程。对于通过径向速度和运输等间接技术检测到的系统，此类测量很具有挑战性，该系统仅针对少数系统进行了测量。我们的目的是在$π$ mensae系统中对外行星的轨道几何形状进行限制，这是G0V恒星18.3 PC主机的主机，可容纳宽大的超级jovian（$ m \ sin i = 10.02 \ pm0.15 \ pm0.15 $ $ m $ m _ {\ rm jup} $ a {\ rm rm jup} $），并具有5.7年度的超级跨度 - （$ m = 4.82 \ pm0.85 $ $ $ m_ \ oplus $）在6.3-d期间。我们将来自河马和Gaia卫星的天文测量与精确确定的光谱轨道结合在一起，以限制外行星轨道平面的倾斜度。我们测量了$ i_b = 49.9 _ { - 4.5}^{+5.3} $ deg的倾斜度，用于$π$ mensae b的轨道平面，导致其质量直接衡量其质量为$ 13.01 _ { - 0.95}^{+1.03}^{+1.03} $ $ M _ {$ m _ {我们发现这两个行星的轨道平面之间有着显着的相互倾斜。 $ i _ {\ rm mut} $的95％可靠间隔在$ 34.5^\ circ $和$ 140.6^\ circ $之间，考虑到$π$ mensae c的轨道的未知位置角度，在该系统内的两个行星都大大排除了co-mensae c的未知位置角度。所有轨道在当今的配置中都是稳定的，而行星C偏心率的世俗振荡被一般相对论的进攻消除了。行星C可能经历了由Kozai-Lidov循环触发的高偏心潮汐迁移，但是涉及磁盘迁移或原位形成的动态历史并未排除。尽管如此，该系统提供了第一个直接的证据，表明具有巨大相互倾向的巨型行星在某些超级地铁系统的起源和演变中起着作用。
Measuring the geometry of multi-planet extrasolar systems can provide insight into their dynamical history and the processes of planetary formation. Such measurements are challenging for systems detected through indirect techniques such as radial velocity and transit, having only been measured for a handful of systems to-date. We aimed to place constraints on the orbital geometry of the outer planet in the $π$ Mensae system, a G0V star at 18.3 pc host to a wide-orbit super-jovian ($M\sin i = 10.02\pm0.15$ $M_{\rm Jup}$) with a 5.7-year period and an inner transiting super-earth ($M=4.82\pm0.85$ $M_\oplus$) with a 6.3-d period. We combined astrometric measurements from the Hipparcos and Gaia satellites with a precisely determined spectroscopic orbit in an attempt to constrain the inclination of the orbital plane of the outer planet. We measured an inclination of $i_b=49.9_{-4.5}^{+5.3}$ deg for the orbital plane of $π$ Mensae b, leading to a direct measurement of its mass of $13.01_{-0.95}^{+1.03}$ $M_{\rm Jup}$. We found a significant mutual inclination between the orbital planes of the two planets; a 95% credible interval for $i_{\rm mut}$ of between $34.5^\circ$ and $140.6^\circ$ after accounting for the unknown position angle of the orbit of $π$ Mensae c, strongly excluding a co-planar scenario for the two planets within this system. All orbits are stable in the present-day configuration, and secular oscillations of planet c's eccentricity are quenched by general relativistic precession. Planet c may have undergone high eccentricity tidal migration triggered by Kozai-Lidov cycles, but dynamical histories involving disk migration or in situ formation are not ruled out. Nonetheless, this system provides the first direct evidence that giant planets with large mutual inclinations have a role to play in the origins and evolution of some super-Earth systems.
