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Uncovering the occurrence rate of terrestrial planets within the HabitableZone (HZ) of their host stars has been a particular focus of exoplanetaryscience in recent years. The statistics of these occurrence rates have largelybeen derived from transiting planet discoveries, and have uncovered numerous HZplanets in compact systems around M dwarf host stars. Here we explore the widthof the HZ as a function of spectral type, and the dynamical constraints on thenumber of stable orbits within the HZ for a given star. We show that, althoughthe Hill radius for a given planetary mass increases with larger semi-majoraxis, the width of the HZ for earlier-type stars allows for more terrestrialplanets 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, weconsider the case of Beta CVn, a nearby bright solar-type star. We present 20years of radial velocities (RV) from the Keck/HIRES and APF instruments andconduct an injection-recovery analysis of planetary signatures in the data. Ouranalysis of these RV data rule out planets more massive than Saturn within10~AU of the star. These system properties are used to calculate the potentialdynamical packing of terrestrial planets in the HZ and show that such nearbystellar targets could be particularly lucrative for HZ planet detection bydirect imaging exoplanet missions.

Dynamical Packing in the Habitable Zone: The Case of Beta CVn