A Perfect Tidal Storm: HD 104067 Planetary Architecture Creating an Incandescent World (2403.17062v2)

Abstract: The discovery of planetary systems beyond the solar system has revealed a diversity of architectures, most of which differ significantly from our system. The initial detection of an exoplanet is often followed by subsequent discoveries within the same system as observations continue, measurement precision is improved, or additional techniques are employed. The HD 104067 system is known to consist of a bright K dwarf host star and a giant planet in a $\sim$55 day period eccentric orbit. Here we report the discovery of an additional planet within the HD 104067 system, detected through the combined analysis of radial velocity data from the HIRES and HARPS instruments. The new planet has a mass similar to Uranus and is in an eccentric $\sim$14 day orbit. Our injection-recovery analysis of the radial velocity data exclude Saturn-mass and Jupiter-mass planets out to 3 AU and 8 AU, respectively. We further present TESS observations that reveal a terrestrial planet candidate ($R_p = 1.30\pm0.12$ $R_\oplus$) in a $\sim$2.2~day period orbit. Our dynamical analysis of the three planet model shows that the two outer planets produce significant eccentricity excitation of the inner planet, resulting in tidally induced surface temperatures as high as $\sim$2600 K for an emissivity of unity. The terrestrial planet candidate may therefore be caught in a tidal storm, potentially resulting in its surface radiating at optical wavelengths.

• The paper identifies a giant planet in a 13.9-day eccentric orbit using high-precision RV measurements from HIRES and HARPS.
• The paper detects an inner terrestrial candidate with a 1.30 Earth radii size and a 2.2-day orbit through detailed TESS analysis and injection-recovery simulations.
• The paper demonstrates that tidal dynamics can raise the inner planet's temperature to around 2600 K, underlining the significant impact of gravitational interactions.

Analysis of the HD 104067 Planetary System: An Incandescent World Shaped by Tidal Dynamics

The paper presented by Kane et al. details an intensive observational and theoretical paper of the exoplanetary system around HD 104067, a K dwarf located approximately 20 parsecs away. The investigation unveils a complex planetary architecture characterized by significant tidal interactions, leading to notable impacts on the potential surface properties of an inner terrestrial planet candidate. Through meticulous analysis involving both radial velocity (RV) measurements and photometric observations, the authors provide substantial evidence supporting the existence and dynamical properties of the involved bodies.

Key Findings and Methodology

1. Radial Velocity Observations: The paper employs high-precision RV data from the HIRES and HARPS instruments, highlighting an efficient methodology to detect and characterize additional planetary bodies in known systems. The data confirms the presence of a giant planet with a Uranus-like mass (planet c) in a 13.9-day eccentric orbit.
2. Detection of an Inner Terrestrial Candidate: Through an analysis of Transiting Exoplanet Survey Satellite (TESS) data, a terrestrial planet candidate with a radius of approximately 1.30 Earth radii is identified in a tight, 2.2-day orbit. The detection leverages both radial velocity stability tests and injection-recovery simulations to assess the sensitivity of detection methods and eliminate the possibility of additional undiscovered massive companions in the system.
3. Dynamical Integration and Tidal Heating Analysis: A significant portion of the paper explores the dynamical simulations performed to assess orbital stability and potential tidal effects. Using the Mercury Integrator Package, simulations predict long-term stability for the system, while quantifying eccentricity-related interactions and their effect on tidal heating of the inner planet candidate.
4. Surface Temperature Implications: Calculations indicate that tides induced by the outer giant planets could elevate the surface temperature of the inner terrestrial candidate to values as high as 2600 K, potentially resulting in a molten state and incidental emission in visible spectra.

Implications and Speculations

• Tidal Heating and Atmospheric Characterization: The paper robustly implicates tidal dynamics as a critical factor in determining planetary surface conditions, potentially leading to observable signatures. Such signatures may serve as markers for similar assessments in other exoplanetary contexts.
• Prospecting Future Observations: The research outlines several observational pathways, including high-precision RV follow-up and high-resolution imaging, to confirm the candidate's planetary status and further understand the system's architecture. This prospect signals opportunities for advancing technology in direct imaging and RV precision enhancements as important tools in exoplanet science.
• Impact on Theoretical Modeling: The dynamical interactions observed in this system challenge existing models of planet evolution and system formation, primarily when extreme tidal interactions play a significant role. The paper underscores the importance of incorporating detailed tidal dynamics into models predicting planetary habitability and atmospheric conditions.

In essence, the paper on the HD 104067 system enriches our understanding of planetary dynamics and the consequential effects of gravitational interactions on planetary atmospheres and surfaces. It exemplifies the intersection of observational astronomy and theoretical modeling, offering insights that are crucial for advancing our comprehension of diverse planetary systems across the galaxy.