General relativistic precession and the long-term stability of the solar system
General relativistic precession and the long-term stability of the solar system
复制标题
广义相对论进动与太阳系的长期稳定性
DOI：
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发表时间：
2023
影响因子：
4.8
通讯作者：
H. Rein
中科院分区：
文献类型：
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作者：
Garett Brown;H. Rein
太阳系的长期演化是混乱的。在某些情况下，长期共振重叠引起的混沌扩散会增加行星进入线性长期共振时的偏心率，从而导致系统不稳定。之前的工作表明，在太阳系建模时，考虑广义相对论对行星进动频率的贡献至关重要。它将太阳系在 5 Gyr 内不稳定的可能性降低了 60 倍。我们对太阳系进行了 1280 个额外的 N 体模拟，跨度为 12.5 Gyr，其中我们允许 GR 进动率随时间变化。我们开发了一个简单、统一的福克-普朗克平流扩散模型，可以重现水星在有、没有或有时变 GR 进动的情况下的不稳定时间。我们表明，虽然忽略广义相对论进动确实使水星的进动频率更接近与木星的共振，但这本身并不能解释不稳定率的增加。扩散速率也有必要显着增加。我们发现系统对进动频率的变化响应平稳：不存在临界 GR 进动频率，低于该频率太阳系会变得更加不稳定。我们的结果表明，平流扩散模型可以很好地描述太阳系的长期演化。
The long-term evolution of the solar system is chaotic. In some cases, chaotic diffusion caused by an overlap of secular resonances can increase the eccentricity of planets when they enter into a linear secular resonance, driving the system to instability. Previous work has shown that including general relativistic contributions to the planets’ precession frequency is crucial when modelling the solar system. It reduces the probability that the solar system destabilizes within 5 Gyr by a factor of 60. We run 1280 additional N-body simulations of the solar system spanning 12.5 Gyr where we allow the GR precession rate to vary with time. We develop a simple, unified, Fokker-Planck advection-diffusion model that can reproduce the instability time of Mercury with, without, and with time-varying GR precession. We show that while ignoring GR precession does move Mercury’s precession frequency closer to a resonance with Jupiter, this alone does not explain the increased instability rate. It is necessary that there is also a significant increase in the rate of diffusion. We find that the system responds smoothly to a change in the precession frequency: There is no critical GR precession frequency below which the solar system becomes significantly more unstable. Our results show that the long-term evolution of the solar system is well described with an advection-diffusion model.