论文标题
最小质量的质量星云：关于固体磁盘轮廓的多样性
Debiasing the Minimum-Mass Extrasolar Nebula: On the Diversity of Solid Disk Profiles
论文作者
论文摘要
原位行星形成理论中的一个基本思想是“最小质量质量外星云”（MMEN），这是在当前位置形成行星所必需的磁盘固体的表面密度剖面（$σ$）。尽管大多数先前的研究都适合观察到的合奏中的所有系属型范围，但目前尚不清楚大多数系外行星系统是否是从通用磁盘模板中形成的。我们使用高级统计模型来用于多个系统系统的基础体系结构来重建MMEN。模拟的物理和开普勒观察到的目录使我们能够直接评估检测偏见的作用，尤其是非传输或未检测到的行星的作用，在改变推断的MMEN方面。我们发现，将$σ=σ_0^*（a/a_0）^β$的幂律与每个多行星系统的形式拟合，从而导致磁盘轮廓的广泛分布； $σ_0^* = 336 _ { - 291}^{+727} $ g/cm $ $^2 $和$β= -1.98 _ { - 1.52}^{+1.55} {+1.55} $包含16-84个百分位数的$ iS_ $ as $ = 0. $ s pransivation $ a $ s pransivati au。大约一半的内行星形成磁盘的最低固体质量为$ \ gtrsim 40 m_ \ oplus $在1 au中。尽管过境观察结果并不倾向于中位数$β$，但它们可能会导致明显的过度估计和低估的$σ_0^*$，从而扩大了磁盘质量的推断分布。然而，检测偏见无法解释观察到的磁盘轮廓的全部差异；如果所有行星原地形成，则没有通用的媒介。固体磁盘轮廓的大量多样性表明，行星系统的大量部分（$ \ gtrsim 23 \％$）经历了移民历史。
A foundational idea in the theory of in situ planet formation is the "minimum mass extrasolar nebula" (MMEN), a surface density profile ($Σ$) of disk solids that is necessary to form the planets in their present locations. While most previous studies have fit a single power-law to all exoplanets in an observed ensemble, it is unclear whether most exoplanetary systems form from a universal disk template. We use an advanced statistical model for the underlying architectures of multi-planet systems to reconstruct the MMEN. The simulated physical and Kepler-observed catalogs allows us to directly assess the role of detection biases, and in particular the effect of non-transiting or otherwise undetected planets, in altering the inferred MMEN. We find that fitting a power-law of the form $Σ= Σ_0^* (a/a_0)^β$ to each multi-planet system results in a broad distribution of disk profiles; $Σ_0^* = 336_{-291}^{+727}$ g/cm$^2$ and $β= -1.98_{-1.52}^{+1.55}$ encompass the 16th-84th percentiles of the marginal distributions in an underlying population, where $Σ_0^*$ is the normalization at $a_0 = 0.3$ AU. Around half of inner planet-forming disks have minimum solid masses of $\gtrsim 40 M_\oplus$ within 1 AU. While transit observations do not tend to bias the median $β$, they can lead to both significantly over- and under-estimated $Σ_0^*$ and thus broaden the inferred distribution of disk masses. Nevertheless, detection biases cannot account for the full variance in the observed disk profiles; there is no universal MMEN if all planets formed in situ. The great diversity of solid disk profiles suggests that a substantial fraction ($\gtrsim 23\%$) of planetary systems experienced a history of migration.
