地球质量行星周围紧密堆积卫星系统的潮汐演化
Tidal evolution of packed moon systems around an Earth-mass planet
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中文总结 AI 辅助
研究地球质量行星周围紧密堆积卫星系统的潮汐演化，用REBOUND N体积分器及相关模块，在多种潮汐耗散参数下评估稳定性，发现地球质量行星可稳定容纳不同质量卫星数，其多卫星系统的存在依赖潮汐耗散，十亿年尺度下潮汐要更弱。
中文摘要 AI 辅助
长期以来，任务一直以其主恒星宜居区内的类地系外行星为目标，随着下一代天基天文台达到探测凌星信号所需的光度灵敏度，系外卫星候选体数量预计会增加。因此，限制紧密堆积卫星系统的稳定性极限对于凌星搜索和预测类地行星周围卫星数量至关重要。在我们的太阳系中，只有三颗卫星环绕类地行星运行，这引发了地球质量系外行星系统是否能维持长期紧密堆积卫星的问题。我们研究了一颗环绕太阳质量恒星运行的地球质量行星的稳定性极限，该行星拥有多颗卫星。我们使用REBOUND N体积分器以及REBOUNDx中的tides_spin模块，在一系列潮汐耗散参数范围内评估月球、冥王星和谷神星质量卫星紧密堆积系统的稳定性，直至最内侧卫星的$10^{7}$个动力学轨道。我们发现，地球质量的行星最多可以稳定容纳两颗月球质量的卫星、三颗冥王星质量的卫星或五颗谷神星质量的卫星。在类似地球的耗散情况下，月球、冥王星和谷神星的紧密堆积系统在狭窄的轨道间距区域内得以存续。这些结果表明，地球质量行星周围存在长期的多卫星系统是可能的，但强烈依赖于潮汐耗散；要使这些结构在十亿年的时间尺度上存在，潮汐必须比当今地月系统的潮汐弱。
英文摘要
While missions have long targeted terrestrial exoplanets within the habitable zone of their host stars, the number of exomoon candidates is expected to grow as next generation space-based observatories achieve the photometric sensitivity required to detect their transit signals. Constraining the stability limits of tightly packed moon systems is therefore essential for transit searches and predicting the number of moons around terrestrial planets. In our Solar System, only three moons orbit the terrestrial planets, motivating the question of whether Earth-mass exoplanet systems can sustain long-lived, tightly packed satellites. We investigate the stability limits of an Earth-mass planet orbiting a Sun-mass star, where the planet hosts multiple moons. We use the REBOUND N-body integrator along with the tides_spin module in REBOUNDx to assess the stability of tightly packed systems of Luna-, Pluto-, and Ceres-mass moons across a range of tidal dissipation parameters, up to $10^{7}$ dynamical orbits of the innermost moon. We find that an Earth-mass planet can stably host up to two Luna-mass moons, three Pluto-mass moons, or five Ceres-mass moons. Under Earth-like dissipation, the Luna, Pluto, and Ceres packed systems survive within narrow regions of orbital spacing. These results imply that long-lived multi-moon systems around Earth-mass planets are possible but strongly depend on tidal dissipation; for these architectures to exist on billion-year timescales, tides must be weaker than those of the present-day Earth-Moon system.
