论文标题
结合运输和RV：合成的种群模型
Combining Transit and RV: A Synthesized Population Model
论文作者
论文摘要
我们提出了一个框架，用于通过同时综合径向速度和过境调查的约束来估计外球星的发生率。我们采用近似贝叶斯计算和各种质量 - 拉迪乌斯（M-R）关系来探索描述这些调查的人群模型，无论是分别拟合还是拟合。使用这种方法，我们符合表单$ d^{2} n/d \ log {p} d \ log {m} \ propto p^βm^α$的行星分布函数，并在$ m_ {b} $中损坏了Power Law in Power Law in $ m_ {b} $，以planters od fgk lating flgk plants plants od fgk plants plants $ p = [25，$ p = [25，200，$ p = [25，200，$]， m _ {\ oplus} $。我们发现来自Otegi等人的M-R关系。 （2020年），使岩石和挥发性丰富的人口重叠的质量，使我们能够找到与两种类型的调查一致的模型。我们的关节拟合给出$ m_ {b} = 21.6 _ { - 3.2}^{+2.5} m _ {\ oplus} $（错误反映了68.3％可靠的间隔）。这几乎比只有途中的考虑因素的突破和没有这样重叠的M-R关系的三个因素。相应的行星星质量比断裂$ q_ {b} \ sim 7 \ times10^{ - 5} $可能与微透镜研究一致（$ q_b \ sim 6 \ sim 6 \ times10^{ - 5} -2 \ 2 \ times1010^{ - 4} $）。关节拟合还要求$ f _ {\ text {rocky}} = 0.63 _ { - 0.04}^{+0.04} $行星的一小部分属于洛基人群。我们的结果强烈表明，未来的M-R关系应解释不同类型的行星的混合，以描述观察到的行星人群。
We present a framework for estimating exoplanet occurrence rates by synthesizing constraints from radial velocity and transit surveys simultaneously. We employ approximate Bayesian computation and various mass-radius (M-R) relations to explore the population models describing these surveys, both separately and in a joint fit. Using this approach, we fit a planet distribution function of the form $d^{2} N/d\log{P}d\log{M} \propto P^β M^α$, with a break in the power law in mass at $M_{b}$, to planets orbiting FGK stars with periods $P = [25, 200]$ days and masses $M = [2, 50] M_{\oplus}$. We find that the M-R relation from Otegi et al. (2020), which lets rocky and volatile-rich populations overlap in mass, allows us to find a model that is consistent with both types of surveys. Our joint fit gives $M_{b} = 21.6_{-3.2}^{+2.5} M_{\oplus}$ (errors reflect 68.3% credible interval). This is nearly a factor of three higher than the break from transit-only considerations and an M-R relation without such an overlap. The corresponding planet-star mass ratio break $q_{b} \sim 7\times10^{-5}$ may be consistent with microlensing studies ($q_b \sim 6\times10^{-5} - 2\times10^{-4}$). The joint fit also requires that a fraction of $F_{\text{rocky}} = 0.63_{-0.04}^{+0.04}$ planets in the overlap region belong to the rocky population. Our results strongly suggest that future M-R relations should account for a mixture of distinct types of planets in order to describe the observed planet population.
