通过太阳系外辐射云中的共振特征探测系外地球和超级地球
The Detectability of Exo-Earths and Super-Earths Via Resonant Signatures in Exozodiacal Clouds
摘要：
直接拍摄太阳系外的类地行星必然意味着要与太阳系外尘埃的天体物理噪音和这些行星在太阳系外云层中产生的共振结构作斗争。使用定制的混合辛积分器，我们已经构建了120个模型的共振结构所创建的外地球和超级地球的圆形轨道相互作用的无碰撞的稳态尘埃云周围的类太阳恒星。我们的模型包括足够的粒子，以克服以前模拟的局限性，这些局限性通常由少数长寿命粒子主导，使我们能够定量研究所得环结构的对比度。我们发现，在圆形轨道上的行星的情况下，对于一个给定的恒星和尘埃源的分布，共振结构的形态和对比度只取决于两个参数：行星质量和$\sqrt{a_{\rm p}}/β$，其中$a_{\rm p}$是行星的半长轴和$β$是辐射压力的比例，重力颗粒。我们构建了25，000个粒子的多粒度模型，并表明在无碰撞的云中，Dohnanyi破碎定律产生了一个共振环，其光学深度由分布中最大的颗粒而不是最小的颗粒主导。我们使用这些模型来估计质量最低的行星的质量，可以通过对尘埃云和行星轨道的各种假设的共振环的观测来检测。我们的模拟表明，质量小到几倍火星的质量的行星可能会产生可检测的签名，在碎片磁盘的半长轴大于10 AU。
英文摘要：
Directly imaging extrasolar terrestrial planets necessarily means contending with the astrophysical noise of exozodiacal dust and the resonant structures created by these planets in exozodiacal clouds. Using a custom tailored hybrid symplectic integrator we have constructed 120 models of resonant structures created by exo-Earths and super-Earths on circular orbits interacting with collisionless steady-state dust clouds around a Sun-like star. Our models include enough particles to overcome the limitations of previous simulations that were often dominated by a handful of long-lived particles, allowing us to quantitatively study the contrast of the resulting ring structures. We found that in the case of a planet on a circular orbit, for a given star and dust source distribution, the morphology and contrast of the resonant structures depend on only two parameters: planet mass and $\sqrt{a_{\rm p}}/β$, where $a_{\rm p}$ is the planet's semi-major axis and $β$ is the ratio of radiation pressure force to gravitational force on a grain. We constructed multiple-grain-size models of 25,000 particles each and showed that in a collisionless cloud, a Dohnanyi crushing law yields a resonant ring whose optical depth is dominated by the largest grains in the distribution, not the smallest. We used these models to estimate the mass of the lowest-mass planet that can be detected through observations of a resonant ring for a variety of assumptions about the dust cloud and the planet's orbit. Our simulations suggest that planets with mass as small as a few times Mar's mass may produce detectable signatures in debris disks for semi-major axes greater than 10 AU.
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