围绕ε Eridani b的潮汐加热系外卫星：可观测性与表征前景
Tidally Heated Exomoons around $ε$ Eridani b: Observability and prospects for characterization
AI总结：
本文通过耦合热-潮汐模型研究ε Eridani b周围潮汐加热系外卫星在MIRI/JWST红外波段的可观测性，并利用可探测性约束其轨道偏心率和内部熔融结构。
摘要：
系外卫星预计会像太阳系行星的卫星一样围绕气态巨行星运行。潮汐加热存在于太阳系卫星中，并且根据其轨道和内部性质，可以加热卫星内部。我们旨在确定潮汐加热系外卫星（THEM）的轨道参数空间，使其能够利用MIRI/JWST在红外波段围绕ε Eridani b被观测到。我们研究在红外波段成功探测到THEM可能对轨道偏心率和内部性质带来的约束。我们还研究了为了施加这些约束，需要独立已知哪些系外卫星性质。我们使用一个耦合的热-潮汐模型来寻找潮汐产生的热量与卫星内部传输的热量之间的稳定平衡点。对于后者，我们考虑一个球形且径向对称的卫星，热量通过熔融亚层（软流圈）中的岩浆平流和下地幔中的对流进行传输。我们纳入内部和潮汐模型参数的不确定性，以评估可通过MIRI观测到的模拟卫星比例。我们发现，一颗以0.02的偏心率围绕ε Eridani b运行的2 R_Io潮汐加热系外卫星，需要具有4倍行星洛希半径的半长轴，才能使100%的模拟产生可观测的卫星。这些值与太阳系气态巨行星卫星的轨道性质相当。我们对高达0.1的偏心率施加了类似的约束。我们得出结论：如果卫星的半长轴和半径已知（例如通过系外卫星凌星），潮汐耗散可以约束卫星的轨道偏心率和内部性质，例如熔融的存在以及含熔融亚层的厚度。
英文摘要：
Exomoons are expected to orbit gas giant exoplanets just as moons orbit solar system planets. Tidal heating is present in solar system satellites and it can heat up their interior depending on their orbital and interior properties. We aim to identify a Tidally Heated Exomoon's (THEM) orbital parameter space that would make it observable in infrared wavelengths with MIRI/JWST around $ε$ Eridani b. We study the possible constraints on orbital eccentricity and interior properties that a successful THEM detection in infrared wavelengths can bring. We also investigate what exomoon properties need to be independently known in order to place these constraints. We use a coupled thermal-tidal model to find stable equilibrium points between the tidally produced heat and heat transported within a moon. For the latter, we consider a spherical and radially symmetric satellite with heat being transported via magma advection in a sub-layer of melt (asthenosphere) and convection in the lower mantle. We incorporate uncertainties in the interior and tidal model parameters to assess the fraction of simulated moons that would be observable with MIRI. We find that a $2 R_{Io}$ THEM orbiting $ε$ Eridani b with an eccentricity of 0.02, would need to have a semi-major axis of 4 planetary Roche-radii for 100% of the simulations to produce an observable moon. These values are comparable with the orbital properties of gas giant solar system satellites. We place similar constraints for eccentricities up to 0.1. We conclude that if the semi-major axis and radius of the moon are known (eg. with exomoon transits), tidal dissipation can constrain the orbital eccentricity and interior properties of the satellite, such as the presence of melt and the thickness of the melt containing sub-layer.
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