Aims. Evidence of mutually inclined planetary orbits has been reported for giant planets in recent years. Here we aim to study the impact of eccentric and inclined massive giant planets on the terrestrial planet formation process, and investigate whether it can possibly lead to the formation of inclined terrestrial planets. Methods. We performed 126 simulations of the late-stage planetary accretion in eccentric and inclined giant planet systems. The physical and orbital parameters of the giant planet systems result from n-body simulations of three giant planets in the late stage of the gas disc, under the combined action of Type II migration and planet-planet scattering. Fourteen two- and three-planet configurations were selected, with diversified masses, semi-major axes (resonant configurations or not), eccentricities, and inclinations (including coplanar systems) at the dispersal of the gas disc. We then followed the gravitational interactions of these systems with an inner disc of planetesimals and embryos (nine runs per system), studying in detail the final configurations of the formed terrestrial planets. Results. In addition to the well-known secular and resonant interactions between the giant planets and the outer part of the disc, giant planets on inclined orbits also strongly excite the planetesimals and embryos in the inner part of the disc through the combined action of nodal resonance and the Lidov–Kozai mechanism. This has deep consequences on the formation of terrestrial planets. While coplanar giant systems harbour several terrestrial planets, generally as massive as the Earth and mainly on low-eccentric and low-inclined orbits, terrestrial planets formed in systems with mutually inclined giant planets are usually fewer, less massive (<0.5 M _(⊕)), and with higher eccentricities and inclinations. This work shows that terrestrial planets can form on stable inclined orbits through the classical accretion theory, even in coplanar giant planet systems emerging from the disc phase.
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机译：目的近年来，已经报道了巨行星相互倾斜的行星轨道的证据。在这里，我们旨在研究偏心和倾斜的巨型巨型行星对地球行星形成过程的影响，并研究它是否可能导致倾斜的地球行星的形成。方法。我们对偏心和倾斜巨型行星系统中的后期行星增生进行了126次模拟。巨型行星系统的物理和轨道参数是由气碟后期对三颗巨型行星进行的n体模拟得出的，这些模拟是在II型迁移和行星行星散射的共同作用下进行的。选择了14种2行星和3行星的构型，在气碟分散处具有多种多样的质量，半长轴（是否有共振构型），偏心率和倾斜度（包括共面系统）。然后，我们跟踪了这些系统与内部小行星和胚胎圆盘的引力相互作用（每个系统9个行程），详细研究了形成的地球行星的最终构造。结果。除了众所周知的巨型行星与圆盘外部之间的世俗和共振相互作用外，倾斜轨道上的巨型行星还通过节点共振和共振的共同作用，强烈激发了圆盘内部的小行星和胚胎。 Lidov–Kozai机制。这对地球行星的形成具有深远的影响。虽然共面的巨型系统具有几个地球行星，通常与地球一样大，并且主要位于低偏心率和低倾斜轨道上，但在具有相互倾斜的巨型行星的系统中形成的陆地行星通常较少，质量较小（<0.5 M _（⊕ ）），并且偏心率和倾斜度更高。这项工作表明，即使在碟状相出现的共面巨型行星系统中，也可以通过经典的吸积理论在稳定的倾斜轨道上形成地行星。
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