论文标题
雪线周围的行星形成。 ii。灰尘还是卵石？
Planetesimal formation around the snow line. II. Dust or pebbles?
论文作者
论文摘要
在雪线周围，冰冷的鹅卵石和硅酸盐灰尘可能会在本地堆积，并通过流媒体不稳定和/或引力不稳定形成冰冷的岩石行星。我们执行1D扩散 - 辅助模拟，其中包括对径向漂移的后反应和冰冻卵石的扩散和硅酸盐的灰尘，冰升华，硅酸盐灰尘的释放以及它们通过再持续的回收利用并粘在雪线外面的卵石上。我们使用了从Ida等人获得的硅酸盐灰尘的尺度高度的现实描述。以及鹅卵石的影响，包括开尔文 - 螺旋菌不稳定性的影响。我们研究固体堆积对径向和垂直方向上湍流的不同有效粘性参数的依赖性（$α_ {\ rm dr} $和$α_ {\ rm dz} $），以及对star（$α__ {\ rm acc acc} $）的气体积聚以及peb y y y y y y y y y y y y y y y y y y y y y y y y y y y y y y y，以及（$ f _ {\ rm p/g} $）。我们得出漂流冰上卵石的升华宽度，这是表征雪线周围硅酸盐灰尘和卵石的堆积的关键参数。 We identify a parameter space (in the $F_{\rm p/g}-α_{\rm acc}-α_{\rm Dz}(=α_{\rm Dr})$ space) where pebbles no longer drift inward to reach the snow line due to the back-reaction that slows down radial velocity of pebbles.我们表明，雪线周围的固体堆积发生在$α_ {\ rm acc} = 10^{ - 3} $的更广泛的参数范围内，而不是$α_ {\ rm acc} = 10^{ - 2} $。上面是关键的$ f _ {\ rm p/g} $值，雪线内的硅酸盐灰尘堆积在$α_ {\ rm dr}/α_ {\ rm dr}/α_ {\ rm acc} \ ll 1 $中，而在雪线之外的pebbles则是$ a casc}/rmm prem premm。 1 $。我们的结果表明，独特的进化路径可以在雪线周围的行星形成方面产生多样的结果。
Around the snow line, icy pebbles and silicate dust may locally pile-up and form icy and rocky planetesimals via streaming instability and/or gravitational instability. We perform 1D diffusion-advection simulations that include the back-reaction to radial drift and diffusion of icy pebbles and silicate dust, ice sublimation, release of silicate dust, and their recycling through recondensation and sticking onto pebbles outside the snow line. We use a realistic description of the scale height of silicate dust obtained from Ida et al. and that of pebbles including the effects of a Kelvin-Helmholtz instability. We study the dependence of solid pile-up on distinct effective viscous parameters for turbulent diffusions in the radial and vertical directions ($α_{\rm Dr}$ and $α_{\rm Dz}$) and for the gas accretion to the star ($α_{\rm acc}$) as well as that on the pebble-to-gas mass flux ($F_{\rm p/g}$). We derive the sublimation width of drifting icy pebbles which is a critical parameter to characterize the pile-up of silicate dust and pebbles around the snow line. We identify a parameter space (in the $F_{\rm p/g}-α_{\rm acc}-α_{\rm Dz}(=α_{\rm Dr})$ space) where pebbles no longer drift inward to reach the snow line due to the back-reaction that slows down radial velocity of pebbles. We show that the pile-up of solids around the snow line occurs in a broader range of parameters for $α_{\rm acc}=10^{-3}$ than for $α_{\rm acc}=10^{-2}$. Above a critical $F_{\rm p/g}$ value, the runaway pile-up of silicate dust inside the snow line is favored for $α_{\rm Dr}/α_{\rm acc} \ll 1$, while that of pebbles outside the snow line is favored for $α_{\rm Dr}/α_{\rm acc} \sim 1$. Our results imply that a distinct evolutionary path could produce a diversity of outcomes in terms of planetesimal formation around the snow line.
