论文标题
带有竖琴的Au Mic的一年：我 - 测量两个过境行星的质量
One year of AU Mic with HARPS: I -- measuring the masses of the two transiting planets
论文作者
论文摘要
围绕明亮，年轻的M-warf au mic围绕的两个透射海王星大小的行星的系统为测试行星形成，早期进化和星形星空相互作用的模型提供了独特的机会。但是，宿主恒星的强烈磁活动使测量行星的质量通过径向速度（RV）方法非常具有挑战性。我们使用竖琴光谱仪的91个观测值报告了系统的1年密集监控活动，从而允许对$ \ sim 600 \，\ rm {m \，s^{ - 1}} $ peac-peak-peak-to-peak-to-peak-to-peak-to-peak-to-peak-to-peak-to-peac-pead-peak-to-peak-to-peak-to-peak to-peac-pead-peak-to-peac-pead-pead-pead-pead-pead-pead-peact-peak to Activation诱导的RV变量进行详细建模。我们使用多维高斯工艺框架对它们和行星信号进行建模。我们用$ \ rm {k_b} = 5.8 \ pm 2.5 \，\ rm {m \，s^{ - 1}} $和$ \ rm {k_c} = 8.5 \ pm 2.5 \ pm 2.5 \ pm 2.5 \，\ rm {m \ rm {m \ rm {m，由此产生的质量估算值，$ \ rm {m_b} = 11.7 \ pm 5.0 \，\ rm {m _ {\ rm \ oplus}} $和$ \ rm {m_c} = 22.2 \ pm 6.7 \ pm 6.7 \ pm 6.7 \，\ rm _ \ rm _ {m _ {moby by beim plant plant plane和行星C比以前想象的要密集得多。这些结果与当前的核心标准模型保持紧张。他们认为，这两个行星都具有比预期的小的信封，而两个行星的信封馏分之间的趋势与理论预测的相反。
The system of two transiting Neptune-sized planets around the bright, young M-dwarf AU Mic provides a unique opportunity to test models of planet formation, early evolution, and star-planet interaction. However, the intense magnetic activity of the host star makes measuring the masses of the planets via the radial velocity (RV) method very challenging. We report on a 1-year, intensive monitoring campaign of the system using 91 observations with the HARPS spectrograph, allowing for detailed modelling of the $\sim 600\, \rm{m\,s^{-1}}$ peak-to-peak activity-induced RV variations. We used a multidimensional Gaussian Process framework to model these and the planetary signals simultaneously. We detect the latter with semi-amplitudes of $\rm{K_b} = 5.8 \pm 2.5\, \rm{m\,s^{-1}}$ and $\rm{K_c} = 8.5 \pm 2.5\, \rm{m\, s^{-1}}$, respectively. The resulting mass estimates, $\rm{M_b} = 11.7 \pm 5.0\, \rm{M_{\rm \oplus}}$ and $\rm{M_c} = 22.2 \pm 6.7\, \rm{M_{\rm \oplus}}$, suggest that planet b might be less dense, and planet c considerably denser than previously thought. These results are in tension with the current standard models of core-accretion. They suggest that both planets accreted a H/He envelope that is smaller than expected, and the trend between the two planets' envelope fractions is the opposite of what is predicted by theory.
