论文标题
放气超阵阵：光化学危险对观察到的低质量行星的质量 - 拉迪乌斯关系的影响
Deflating Super-Puffs: Impact of Photochemical Hazes on the Observed Mass-Radius Relationship of Low Mass Planets
论文作者
论文摘要
观察到的低质量行星的质量拉迪乌斯关系使我们对它们的组成和进化的理解。低质量，大半径物体（“超淋浴”）的最新发现挑战了行星形成和大气损失的理论，因为它们的高推断气体使它们容易受到失控的积聚和流体动力逃生的影响。在这里，我们提出，高空光化学危险剂可以增强观察到的低质量行星的半径并解释超高的性质。我们在散发性传染平衡和大气逃生和雾霾分布的计算速率中构建了模型大气，考虑到雾化凝结，沉积，扩散和通过流出风的趋势。 We develop mass-radius diagrams that include atmospheric lifetimes and haze opacity, which is enhanced by the outflow, such that young (~0.1-1 Gyr), warm (T$_{eq}$ $\geq$ 500 K), low mass objects ($M_c$ < 4M$_{\rm Earth}$) should experience the most apparent radius enhancement due to hazes, reaching factors of three.这可以调解最极端超级效果的密度和年龄。对于开普勒-51b，包含HAZES将其推断的气体质量分数降低到<10％，类似于亚纽扣半径间隙的大半径侧的行星。这表明Kepler-51b可能正在向该人群演变，并且一些温暖的亚核病可能是从超级狂暴中演变而来的。 Hazes还提供了超淋浴和子纽扣的传输光谱，这与最近的测量相一致。我们的假设可以通过对中红外波长的超高传输光谱的未来观察结果进行检验，我们预测行星半径将是近红外观察到的一半。
The observed mass-radius relationship of low-mass planets informs our understanding of their composition and evolution. Recent discoveries of low mass, large radii objects ("super-puffs") have challenged theories of planet formation and atmospheric loss, as their high inferred gas masses make them vulnerable to runaway accretion and hydrodynamic escape. Here we propose that high altitude photochemical hazes could enhance the observed radii of low-mass planets and explain the nature of super-puffs. We construct model atmospheres in radiative-convective equilibrium and compute rates of atmospheric escape and haze distributions, taking into account haze coagulation, sedimentation, diffusion, and advection by an outflow wind. We develop mass-radius diagrams that include atmospheric lifetimes and haze opacity, which is enhanced by the outflow, such that young (~0.1-1 Gyr), warm (T$_{eq}$ $\geq$ 500 K), low mass objects ($M_c$ < 4M$_{\rm Earth}$) should experience the most apparent radius enhancement due to hazes, reaching factors of three. This reconciles the densities and ages of the most extreme super-puffs. For Kepler-51b, the inclusion of hazes reduces its inferred gas mass fraction to <10%, similar to that of planets on the large radius side of the sub-Neptune radius gap. This suggests that Kepler-51b may be evolving towards that population, and that some warm sub-Neptunes may have evolved from super-puffs. Hazes also render transmission spectra of super-puffs and sub-Neptunes featureless, consistent with recent measurements. Our hypothesis can be tested by future observations of super-puffs' transmission spectra at mid-infrared wavelengths, where we predict that the planet radius will be half of that observed in the near-infrared.
