论文标题
在原球面磁盘中，鹅卵石堆积的“无饮用”堆积。造成的行星带的特性
A "no-drift" runaway pile-up of pebbles in protoplanetary disks II. Characteristics of the resulting planetesimal belt
论文作者
论文摘要
从鹅卵石形成行星是我们当前对行星形成的理解的主要挑战。在原月经磁盘中，鹅卵石通过煤气阻力向内向内漂移，它们可能进入死区。在这种情况下，我们确定将鹅卵石拖入气体的反应可能导致卵石的失控堆积，即所谓的无饮用机构。我们通过研究所得的行星带的性质和特征来改善对无饮用机制的研究。我们通过包括对卵石的径向漂移的反应，并通过流媒体不稳定性进行了对卵石的径向漂移，对死区外部区域的漂移卵石进行了1D扩散 - 添加模拟。我们考虑了调节磁盘中平面中鹅卵石的气体积聚和垂直搅拌的参数。在这项研究中，将卵石至气体质量通量（$ f _ {\ rm p/g} $）固定为参数。我们发现，最初在狭窄的环内形成的行星，其宽度随着时间的流逝而径向扩散。该系统最终到达稳态，地球皮带的宽度不再发生变化。为具有$ f _ {\ rm p/g} \ gtrsim 0.1 $的磁盘形成了不可忽略的行星图（多个地球质量），以超过$ \ sim 10-100 $ kyr的标称参数：$ \ gtrsim10^$ \ y y y y y y y y y y y y y y rux的气体质量通量： $τ_{\rm s} \simeq 0.01-0.1$, $α_{\rm mid} \lesssim 10^{-4}$, and $α_{\rm acc} \simeq 10^{-3}-10^{-2}$ at $r \lesssim 10$ au, where $r$, $τ_ {\ rm s} $，$α_ {\ rm mid} $，$α_ {\ rm acc} $是地中心距离，stokes数量，stokes数量，且参数是死去区域中的参数，控制了垂直的$ pebbles $ pebbles $ pebbles和scale $ s scile $ s scile＆s scaple的效率 - （即气体表面密度）。
Forming planetesimals from pebbles is a major challenge in our current understanding of planet formation. In a protoplanetary disk, pebbles drift inward near the disk midplane via gas drag and they may enter a dead zone. In this context, we identified that the backreaction of the drag of pebbles onto the gas could lead to a runaway pile-up of pebbles, the so-called no-drift mechanism. We improve upon the previous study of the no-drift mechanism by investigating the nature and characteristics of the resultant planetesimal belt. We performed 1D diffusion-advection simulations of drifting pebbles in the outer region of a dead zone by including the backreaction to the radial drift of pebbles and including planetesimal formation via the streaming instability. We considered the parameters that regulate gas accretion and vertical stirring of pebbles in the disk midplane. In this study, the pebble-to-gas mass flux ($F_{\rm p/g}$) was fixed as a parameter. We find that planetesimals initially form within a narrow ring whose width expands as accumulating pebbles radially diffuse over time. The system finally reaches a steady-state where the width of the planetesimal belt no longer changes. A non-negligible total mass of planetesimals (more than one Earth mass) is formed for a disk having $F_{\rm p/g} \gtrsim 0.1$ for more than $\sim 10-100$ kyr with nominal parameters: a gas mass flux of $\gtrsim10^{-8} {\rm M}_\oplus$/yr, $τ_{\rm s} \simeq 0.01-0.1$, $α_{\rm mid} \lesssim 10^{-4}$, and $α_{\rm acc} \simeq 10^{-3}-10^{-2}$ at $r \lesssim 10$ au, where $r$, $τ_{\rm s}$, $α_{\rm mid}$, and $α_{\rm acc}$ are the heliocentric distance, the Stokes number, and the parameters in a dead zone controlling the efficiencies of vertical turbulent diffusion of pebbles (i.e., scale height of pebbles) and gas accretion of the $α$-disk (i.e., gas surface density), respectively.
