湍流扩散和反作用对两个共振行星周围尘埃分布的影响
Effects of turbulent diffusion and back-reaction on the dust distribution around two resonant planets
摘要：
在演化和尘埃的星周盘中，两颗质量与木星和土星相当的行星向外迁移，同时保持轨道共振，可以在尘埃分布中产生独特的特征。尘埃聚集在共同气体间隙的外缘，这就像一个尘埃陷阱，行星向外运动会显著增加当地的尘埃浓度。与此同时，行星轨道内的尘埃分布中形成了一个扩大的空腔，因为尘埃不能通过共同的气体间隙过滤，该区域的颗粒耗尽通过向内漂移继续。在气体分布中没有空腔，因为气体可以通过间隙过滤，尽管行星上正在进行的气体吸积可以降低内盘中的气体密度。这种行为被证明是通过模拟忽略灰尘扩散的影响，由于湍流和灰尘的气体上的反反应。这两种效应都可以通过使颗粒过滤通过灰尘捕集器来改变间隙外边缘处的灰尘峰和内部灰尘腔的形成。我们进行了高分辨率的流体动力学模拟的气体和尘埃物种的耦合演化，后者被视为无压流体，在两个巨大的行星的存在。我们发现，扩散和逆反应可以改变一些形态方面的尘埃分布，但不改变一些主要特征，如外峰和扩大内腔。这些发现证实了不同的参数化气体粘度。
英文摘要：
In evolved and dusty circumstellar discs, two planets with masses comparable to Jupiter and Saturn that migrate outwards while maintaining an orbital resonance can produce distinctive features in the dust distribution. Dust accumulates at the outer edge of the common gas gap, which behaves as a dust trap, where the local dust concentration is significantly enhanced by the planets outward motion. Concurrently, an expanding cavity forms in the dust distribution inside the planets orbits, because dust does not filter through the common gaseous gap and grain depletion in the region continues via inward drifting. There is no cavity in the gas distribution because gas can filter through the gap, although ongoing gas accretion on the planets can reduce the gas density in the inner disc. Such behaviour was demonstrated by means of simulations neglecting the effects of dust diffusion due to turbulence and of dust backreaction on the gas. Both effects may alter the formation of the dust peak at the gap outer edge and of the inner dust cavity, by letting grains filter through the dust trap. We performed high resolution hydrodynamical simulations of the coupled evolution of gas and dust species, the latter treated as pressureless fluids, in the presence of two giant planets. We show that diffusion and backreaction can change some morphological aspects of the dust distribution but do not alter some main features, such as the outer peak and the expanding inner cavity. These findings are confirmed for different parametrizations of gas viscosity.
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