Abstract
Abstract In this Letter, we measure the full orbital architecture of the two-planet system around the nearby K0 dwarf 14 Herculis. 14 Her (HD 145675, HIP 79248) is a middle-aged ( 4.6 − 1.3 + 3.8 Gyr) K0 star with two eccentric giant planets identified in the literature from radial velocity (RV) variability and long-term trends. Using archival RV data from Keck/HIRES in concert with Gaia-Hipparcos acceleration in the proper motion vector for the star, we have disentangled the mass and inclination of the b planet to 9.1 − 1.1 + 1.0 M Jup and 32.7 − 3.2 + 5.3 degrees. Despite only partial phase coverage for the c planet’s orbit, we are able to constrain its mass and orbital parameters as well to 6.9 − 1.0 + 1.7 M Jup and 101 − 33 + 31 degrees. We find that coplanarity of the b and c orbits is strongly disfavored. Combined with the age of the system and the comparable masses of its planets, this suggests that planet–planet scattering may be responsible for the current configuration of the system.
Highlights
The orbital parameters of a planetary system are sculpted by its formation processes and evolutionary history in a quest for a stable configuration
Our derived stellar and planetary parameters are shown in Despite only seeing a long-term trend in the radial velocity (RV) data covering ∼15% of the period, we can set some constraints on the orbital parameters of the c planet
Introducing the constraint from the absolute astrometry enhances these parameters for the c planet with respect to earlier determinations using only RV data
Summary
The orbital parameters of a planetary system are sculpted by its formation processes and evolutionary history in a quest for a stable configuration. Coplanar planetary orbits are a natural consequence of formation in a disk, whether by core accretion or gravitational instability (e.g., Lissauer 1993; Boss 2001). This effect is observed in the low eccentricities and low mutual inclinations of the solar system planets, and multiexoplanet systems (e.g., Limbach & Turner 2015). The orbital architectures of mature systems reflect both their formation conditions and their dynamical evolution
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