暗夜中的生命：流浪行星卫星的潜在宜居性
Life in the dark: Potential urability of moons of rogue planets
AI总结：
研究探讨流浪行星卫星在超新星爆炸后是否仍能保持束缚，并分析潮汐加热对维持地下液态海洋的作用，发现部分卫星具备长期宜居潜力。
摘要：
自由漂浮的行星被认为在银河系中数量众多，可能在被弹出原生系统后仍保留其卫星。如果这些卫星获得或保持轨道偏心率，潮汐耗散可以提供一个长期的内部热源，可能在没有恒星辐射的情况下创造宜居环境（能够促进生命起源）。我们探讨（i）是否被核心塌缩超新星弹出的卫星仍会束缚于行星上，（ii）爆炸如何重塑它们的轨道，以及（iii）在什么情况下潮汐加热可以维持宜居的地下海洋。我们进行了三维N体模拟，使用第八阶龙格-库塔方案，建模了10个太阳质量前体的同序恒星质量损失。爆炸后单个卫星和共振卫星系统的轨道元素被分析，利用恒定相位滞后模型估计潮汐加热功率，针对几种潮汐耗散函数和卫星密度进行了计算。所有模拟的卫星都存活了超新星并仍束缚于其行星上。爆炸使单个卫星的偏心率增加到约7×10⁻⁴和约3×10⁻³，分别对应于行星圆轨道和偏心轨道的卫星。对于共振对，偏心率保持在≤2×10⁻²。卫星的半长轴变化不超过0.2%。对于12-15%的案例——偏好于轨道半长轴a≤15R_planet且偏心率e≥10⁻³的卫星——特定潮汐加热功率介于欧罗巴或恩克拉多估计值的0.1到10倍之间，足以维持冰壳下的液态海洋。偏心率耗散时间尺度超过太阳系的年龄，对于a≥10R_planet的情况，意味着数亿年持续加热。这些世界代表未来寻找外星生命的有希望的目标。
英文摘要：
Free-floating planets are thought to be numerous in the Galaxy and may retain their moons after ejection from their natal systems. If those satellites acquire or preserve orbital eccentricity, tidal dissipation could provide a long-lasting internal heat source, potentially creating urable environments (capable of enabling abiogenesis) in the absence of stellar radiation. We explore (i) whether moons remain bound to planets expelled by a core-collapse supernova, (ii) how the explosion reshapes their orbits, and (iii) under which circumstances tidal heating can sustain urable subsurface oceans. We carried out three-dimensional N-body simulations with an 8th-order Runge-Kutta scheme, modelling homologous stellar mass loss for progenitors of 10 M$_{\odot}$. Post-explosion orbital elements of single moons and resonant moon systems were analysed, and tidal heating power was estimated with a constant phase-lag model for several tidal dissipation functions and moon densities. All simulated moons survive the supernova and remain bound to their planets. The explosion excites moon eccentricities up to $\sim7\times10^{-4}$ and $\sim3\times10^{-3}$ for single moons of planets with circular and eccentric orbits, respectively. For resonant pairs, an eccentricity of $\leq2\times10^{-2}$ is preserved. The semi-major axis of the moons changes by $\leq0.2\%$. For 12-15\% of cases -- preferentially moons at $a\leq15\,R_{\mathrm{planet}}$ and with $e\geq10^{-3}$ -- the specific tidal heating power lies between 0.1 and 10 times what is estimated on Europa or Enceladus, sufficient to maintain liquid oceans beneath an ice crust. Eccentricity damping timescales exceed the age of the Solar System for $a\geq10\,R_{\mathrm{planet}}$, implying billions of years of continuous heating on the moons. Such worlds represent promising targets for future searches for extraterrestrial life.
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