论文标题
一对经过明亮的K-Dwarf TOI-1064的子纽扣，其特征是Cheops
A pair of Sub-Neptunes transiting the bright K-dwarf TOI-1064 characterised with CHEOPS
论文作者
论文摘要
我们报告了一对传播明亮的K-Warf TOI-1064（TIC 79748331）的子脉冲的发现和表征，该子脉冲最初在苔丝光度法中检测到。为了表征系统，我们执行并检索了Cheops，Tess和地面光度法，HARPS高分辨率光谱和双子体斑点成像。我们表征主机星并确定$ t _ {\ rm eff，\ star} = 4734 \ pm67 $ k，$ r _ {\ star} = 0.726 \ pm0.007 $ $ $ $ $ r _ {\ odot} $，和$ m _ {\ star} = 0.748 \ pm0.748 \ $ odot。我们提出了一种基于PSF形状变化建模的新型降低方法，并证明了其适合纠正Cheops数据中通量变化的适用性。我们确认了这两个身体的行星性质，并发现TOI-1064 B的轨道周期为$ p _ {\ rm b} = 6.44387 \ pm0.00003 $ d，半径为$ r _ {\ rm b} = 2.59 \ 2.59 \ pm0.04 $ $ r _; b} = 13.5 _ { - 1.8}^{+1.7} $ $ m _ {\ oplus} $，而TOI-1064 C的轨道周期为$ p _ {\ rm c} = 12.22657^ C} = 2.65 \ pm0.04 $ $ $ r _ {\ oplus} $，以及3 $σ$上限限制为8.5 $ {\ rm m _ {\ oplus}} $。从高精度光度法中，我们获得了$ \ sim $ 1.6％的半径不确定性，使我们能够进行内部结构和大气逃生建模。 TOI-1064 B是最稠密的，特征良好的亚核，具有微弱的气氛，可以通过迁移到原始圆盘后的原始信封的丧失来解释。由于暂定的低密度，TOI-1064 C可能具有扩展的气氛，但是需要进一步的RV来确认这种情况和类似的半径，该系统的不同质量是该系统的不同质量。 TOI-1064 B的高精度数据和建模对于大摩尔迪乌斯空间区域中的行星很重要，它使我们能够确定大量的巨大亚螺旋体的散装密度恒星金属性的趋势，这可能会暗示这一行星群体的形成。
We report the discovery and characterisation of a pair of sub-Neptunes transiting the bright K-dwarf TOI-1064 (TIC 79748331), initially detected in TESS photometry. To characterise the system, we performed and retrieved CHEOPS, TESS, and ground-based photometry, HARPS high-resolution spectroscopy, and Gemini speckle imaging. We characterise the host star and determine $T_{\rm eff, \star}=4734\pm67$ K, $R_{\star}=0.726\pm0.007$ $R_{\odot}$, and $M_{\star}=0.748\pm0.032$ $M_{\odot}$. We present a novel detrending method based on PSF shape-change modelling and demonstrate its suitability to correct flux variations in CHEOPS data. We confirm the planetary nature of both bodies and find that TOI-1064 b has an orbital period of $P_{\rm b}=6.44387\pm0.00003$ d, a radius of $R_{\rm b}=2.59\pm0.04$ $R_{\oplus}$, and a mass of $M_{\rm b}=13.5_{-1.8}^{+1.7}$ $M_{\oplus}$, whilst TOI-1064 c has an orbital period of $P_{\rm c}=12.22657^{+0.00005}_{-0.00004}$ d, a radius of $R_{\rm c}=2.65\pm0.04$ $R_{\oplus}$, and a 3$σ$ upper mass limit of 8.5 ${\rm M_{\oplus}}$. From the high-precision photometry we obtain radius uncertainties of $\sim$1.6%, allowing us to conduct internal structure and atmospheric escape modelling. TOI-1064 b is one of the densest, well-characterised sub-Neptunes, with a tenuous atmosphere that can be explained by the loss of a primordial envelope following migration through the protoplanetary disc. It is likely that TOI-1064 c has an extended atmosphere due to the tentative low density, however further RVs are needed to confirm this scenario and the similar radii, different masses nature of this system. The high-precision data and modelling of TOI-1064 b are important for planets in this region of mass-radius space, and it allows us to identify a trend in bulk density-stellar metallicity for massive sub-Neptunes that may hint at the formation of this population of planets.
