A super-Earth and a mini-Neptune around Kepler-59

Abstract

We characterize the radii and masses of the star and planets in the Kepler-59 system, as well as their orbital parameters. The star parameters are determined through a standard spectroscopic analysis, resulting in a mass of $1.359\pm 0.155M_{\odot }$ and a radius of $1.367\pm 0.078R_{\odot }$. The planetary radii obtained are $1.5\pm 0.1R_{\oplus }$ for the inner and $2.2\pm 0.1R_{\oplus }$ for the outer planet. The orbital parameters and the planetary masses are determined by the inversion of Transit Timing Variations (TTV) signals. For this, we consider two different data sets, one provided by Holczer et al. 2016, with TTVs only for the planet Kepler-59c, and the other provided by Rowe et al. 2015, with TTVs signals for both planets. The inversion method is carried out by applying an algorithm of Bayesian inference (MultiNest) combined with an efficient N-body integrator (Swift). For each of the data sets, two possible solutions are found, both having the same probability according to their corresponding Bayesian evidences. All four solutions appear to be indistinguishable within their 2-$\sigma$ uncertainties. Nevertheless, statistical analyses show that the solutions from Rowe et al. 2015 data better characterize the data. The first and second solutions identify masses of $5_{-2}^{+4}{M}_{\oplus }$ and $4.6_{-2.0}^{+3.6}{M}_{\oplus }$, and $3.0_{-0.8}^{+0.8}{M}_{\oplus }$ and $2.6_{-0.8}^{+1.9}{M}_{\oplus }$ for the inner and outer planet, respectively. This points to a system with an inner super-Earth and an outer mini-Neptune. Dynamical studies show the planets have almost co-planar orbits with small eccentricities ($e<0.1$), close but not into the 3:2 mean motion resonance. Stability analysis indicates that this configuration is stable over million years of evolution.

arXiv comment10 pages, 7 figures

References in corpus (47)

• The chemical composition of the Sun
• Gaia Data Release 2. Summary of the contents and survey properties
• The Gaia mission
• MultiNest: an efficient and robust Bayesian inference tool for cosmology and particle physics
• MESA Isochrones and Stellar Tracks (MIST). I: Solar-Scaled Models
• Analytic Lightcurves for Planetary Transit Searches
• Gaia Data Release 2: The astrometric solution
• Estimating distances from parallaxes IV: Distances to 1.33 billion stars in Gaia Data Release 2
• The California-Kepler Survey. III. A Gap in the Radius Distribution of Small Planets
• Planetary Candidates Observed by Kepler, III: Analysis of the First 16 Months of Data
• Characteristics of planetary candidates observed by Kepler, II: Analysis of the first four months of data
• Importance Nested Sampling and the MultiNest Algorithm
• Prevalence of Earth-size planets orbiting Sun-like stars
• DHP Framework: Digital Health Passports Using Blockchain -- Use case on international tourism during the COVID-19 pandemic
• On detecting terrestrial planets with timing of giant planet transits
• Mass-Radius Relationships for Solid Exoplanets
• Kepler planets: a tale of evaporation
• Most 1.6 Earth-Radius Planets are not Rocky
• The evaporation valley in the Kepler planets
• Probabilistic Forecasting of the Masses and Radii of Other Worlds
• Growth Model Interpretation of Planet Size Distribution
• Core-powered mass loss and the radius distribution of small exoplanets
• Galactic Reddening in 3D from Stellar Photometry - An Improved Map
• False positive probabilties for all Kepler Objects of Interest: 1284 newly validated planets and 428 likely false positives
• Planetary Candidates Observed by Kepler. VIII. A Fully Automated Catalog With Measured Completeness and Reliability Based on Data Release 25
• Sculpting the Valley in the Radius Distribution of Small Exoplanets as a by-product of Planet Formation: The Core-Powered Mass-Loss Mechanism
• Extracting Planet Mass and Eccentricity From TTV data
• The California-Kepler Survey. I. High Resolution Spectroscopy of 1305 Stars Hosting Kepler Transiting Planets
• Revised Radii of Kepler Stars and Planets Using Gaia Data Release 2
• Super-Earth Atmospheres: Self-Consistent Gas Accretion and Retention
• Asteroseismology and Gaia: Testing Scaling Relations Using 2200 Kepler Stars with TGAS Parallaxes
• Periodograms for Multiband Astronomical Time Series
• Kepler Planet Masses and Eccentricities from TTV Analysis
• Transit Timing Observations from Kepler. IX. Catalog of the Full Long-Cadence Data Set
• Transit Timing Observations from Kepler: VII. Confirmation of 27 planets in 13 multiplanet systems via Transit Timing Variations and orbital stability
• Planetary Candidates Observed by Kepler V: Planet Sample from Q1-Q12 (36 Months)
• The California-Kepler Survey. II. Precise Physical Properties of 2025 Kepler Planets and Their Host Stars
• A Statistical Reconstruction of the Planet Population Around Kepler Solar-Type Stars
• The Detection and Characterization of a Nontransiting Planet by Transit Timing Variations
• KOI-142, the King of Transit Variations, is a Pair of Planets near the 2:1 Resonance
• Mass and Mass Scalings of Super-Earths
• Retired A Stars Revisited: An Updated Giant Planet Occurrence Rate as a Function of Stellar Metallicity and Mass
• A Spectroscopic Analysis of the California-Kepler Survey Sample: I. Stellar Parameters, Planetary Radii and a Slope in the Radius Gap
• Transformations between 2MASS, SDSS and BVRI photometric systems: bridging the near infrared and optical
• Evidence for spatially-correlated $Gaia$ parallax errors in the $Kepler$ field
• Masses of Kepler-46b, c from Transit Timing Variations
• Masses of the Kepler-419 Planets from Transit Timing Variations Analysis

Cited by in corpus (4)

• Dissipative Capture of Planets Into First-Order Mean-Motion Resonances
• Near Mean Motion Resonance of Terrestrial Planet Pair Induced by Giant Planet: Application to Kepler-68 System
• On the importance of wave planet interactions for the migration of two super-Earths embedded in a protoplanetary disk
• Nauyaca: a new tool to determine planetary masses and orbital elements through transit timing analysis