宜居带中的动力学堆积：Beta CVn的情况
Dynamical Packing in the Habitable Zone: The Case of Beta CVn
摘要：
揭示类地行星在其主星宜居带（HZ）内的出现率是近年来系外行星科学的一个特别焦点。这些发生率的统计数据很大程度上来自凌日行星的发现，并在M矮星周围的紧凑系统中发现了许多HZ行星。在这里，我们探讨的宽度的HZ作为一个函数的光谱型，和一个给定的恒星的HZ内的稳定轨道的数量的动力学约束。我们发现，虽然希尔半径为一个给定的行星质量增加较大的半长轴，早期型恒星的HZ的宽度允许更多的类地行星在HZ比晚型恒星。一般来说，动力学约束允许$\sim$ 6 HZ地球质量行星具有恒星质量$\gtrsim 0.7 M_\odot$，具体取决于更远的巨行星的存在。作为一个例子，我们考虑的情况下，β CVn，附近的明亮的太阳型恒星。我们提出了20年的径向速度（RV）从凯克/HIRES和APF仪器，并进行注入回收分析的行星签名的数据。我们对这些RV数据的分析排除了在恒星10天文单位范围内比土星更大的行星。这些系统的属性被用来计算潜在的动态包装的类地行星在HZ和显示，这样的附近的恒星目标可能是特别有利可图的HZ行星探测直接成像系外行星任务。
英文摘要：
Uncovering the occurrence rate of terrestrial planets within the Habitable Zone (HZ) of their host stars has been a particular focus of exoplanetary science in recent years. The statistics of these occurrence rates have largely been derived from transiting planet discoveries, and have uncovered numerous HZ planets in compact systems around M dwarf host stars. Here we explore the width of the HZ as a function of spectral type, and the dynamical constraints on the number of stable orbits within the HZ for a given star. We show that, although the Hill radius for a given planetary mass increases with larger semi-major axis, the width of the HZ for earlier-type stars allows for more terrestrial planets in the HZ than late-type stars. In general, dynamical constraints allow $\sim$6 HZ Earth-mass planets for stellar masses $\gtrsim 0.7 M_\odot$, depending on the presence of farther out giant planets. As an example, we consider the case of Beta CVn, a nearby bright solar-type star. We present 20 years of radial velocities (RV) from the Keck/HIRES and APF instruments and conduct an injection-recovery analysis of planetary signatures in the data. Our analysis of these RV data rule out planets more massive than Saturn within 10~AU of the star. These system properties are used to calculate the potential dynamical packing of terrestrial planets in the HZ and show that such nearby stellar targets could be particularly lucrative for HZ planet detection by direct imaging exoplanet missions.
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