THE MASS OF KOI-94d AND A RELATION FOR PLANET RADIUS, MASS, AND INCIDENT FLUX

By L. Weiss, G. Marcy, J. Rowe, Andrew W. Howard, H. Isaacson, Jon Fortney, N. Miller, B. Demory, Debra A. Fischer, E. Adams and 8 more. 2013

197 citations recorded by the source corpus.

We measure the mass of a modestly irradiated giant planet, KOI-94d. We wish to determine whether this planet, which is in a 22 day orbit and receives 2700 times as much incident flux as Jupiter, is as dense as Jupiter or rarefied like inflated hot Jupiters. KOI-94 also hosts at least three smaller transiting planets, all of which were detected by the Kepler mission. With 26 radial velocities of KOI-94 from the W. M. Keck Observatory and a simultaneous fit to the Kepler light curve, we measure the mass of the giant planet and determine that it is not inflated. Support for the planetary interpretation of the other three candidates comes from gravitational interactions through transit timing variations, the statistical robustness of multi-planet systems against false positives, and several lines of evidence that no other star resides within the photometric aperture. We report the properties of KOI-94b (MP = 10.5 ± 4.6 M⊕, RP = 1.71 ± 0.16 R⊕, P = 3.74 days), KOI-94c (MP = M⊕, RP = 4.32 ± 0.41 R⊕, P = 10.4 days), KOI-94d (MP = 106 ± 11 M⊕, RP = 11.27 ± 1.06 R⊕, P = 22.3 days), and KOI-94e (MP = M⊕, RP = 6.56 ± 0.62 R⊕, P = 54.3 days). The radial velocity analyses of KOI-94b and KOI-94e offer marginal (>2σ) mass detections, whereas the observations of KOI-94c offer only an upper limit to its mass. Using the KOI-94 system and other planets with published values for both mass and radius (138 exoplanets total, including 35 with MP < 150 M⊕), we establish two fundamental planes for exoplanets that relate their mass, incident flux, and radius from a few Earth masses up to 13 Jupiter masses: (RP/R⊕) = 1.78(MP/M⊕)0.53(F/erg s−1 cm−2)−0.03 for MP < 150 M⊕, and RP/R⊕ = 2.45(MP/M⊕)−0.039(F/erg s−1 cm−2)0.094 for MP > 150 M⊕. These equations can be used to predict the radius or mass of a planet.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/d84bade1b4f9cd203ade498f612e14bffeff028e

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Citations in the corpus

Kepler Planet Masses and Eccentricities from TTV Analysis (2016, methodology): “…low-order MMRs with planets c and d. Kepler-89 c and d are among the few planets for which both RV and TTV mass measurements have been reported, with RV mass measurements reported by both Hirano et al. (2012) and Weiss et al. (2013) and a previous TTV measurement reported by Masuda et al. (2013).”
THE TRANSITING EXOPLANET SURVEY SATELLITE: SIMULATIONS OF PLANET DETECTIONS AND ASTROPHYSICAL FALSE POSITIVES (2015, methodology): “To evaluate the detectability of the Doppler signal we assign masses to the simulated planets using the empirical mass-radius relation provided by Weiss et al. (2013).”
A Population Study of Gaseous Exoplanets (2017, background): “These results indicate that planetary surface gravity is a secondary factor in identifying inflated atmospheres (Laughlin et al. 2011; Weiss et al. 2013; Spiegel & Burrows 2013).”
VALIDATION OF KEPLER'S MULTIPLE PLANET CANDIDATES. III. LIGHT CURVE ANALYSIS AND ANNOUNCEMENT OF HUNDREDS OF NEW MULTI-PLANET SYSTEMS (2014, background): “An extreme example is KOI-94 (Kepler-89) (Weiss et al. 2013), which has an effective duty cycle of less than 50% due to its location on the edge of one of the CCD detectors.”
Dearth of short-period Neptunian exoplanets - a desert in period-mass and period-radius planes (2016, methodology): “1, the mass-radius relation is similar to the one used by Matsakos & Konigl (2016), which was based on the relation reported by Weiss et al. (2013).”
WASP-47: A HOT JUPITER SYSTEM WITH TWO ADDITIONAL PLANETS DISCOVERED BY K2 (2015, background): “Measuring the mass of the two planetary companions with RVs could both improve the precision of the inferred masses and test the consistency of TTV and RV masses, between which there is some tension (e.g. KOI 94: Weiss et al. 2013; Masuda et al. 2013).”
PROBABILISTIC FORECASTING OF THE MASSES AND RADII OF OTHER WORLDS (2016, methodology): “Parametric models, in particular power laws, have long been popular for modeling the MR relation with many examples even in the recent literature (e.g., Valencia et al. 2006; Weiss et al. 2013; Hatzes & Rauer 2015; Wolfgang et al. 2015; Zeng et al. 2016).”
KEPLER-413B: A SLIGHTLY MISALIGNED, NEPTUNE-SIZE TRANSITING CIRCUMBINARY PLANET (2014, unknown): “The expected mass is Mp ∼ 16M⊕, using the mass-radius relation of Weiss et al. (2013) for 1M⊕ < M < 150M⊕, whereas our model provides Mp ∼ 67M⊕±21M⊕.”
ALL SIX PLANETS KNOWN TO ORBIT KEPLER-11 HAVE LOW DENSITIES (2013, background): “…the reductions in size estimates, all planets are large for their masses in the sense that they lie above both the Mp/M⊕ ≈ (Rp/R⊕)2.06 relationship that is valid for planets in our solar system (Lissauer et al. 2011b) and mass–radius fits to exoplanets (Wu & Lithwick 2012; Weiss et al. 2013).”
THE MASS–RADIUS RELATION FOR 65 EXOPLANETS SMALLER THAN 4 EARTH RADII (2013, background): “We also include all 40 transiting planets with RV follow-up in Marcy et al. (2014) that are smaller than 4R⊕, and the RVdetermined mass of KOI-94 b (Weiss et al. 2013), none of which yet appear on exoplanets.org.”
WASP-121 b: a hot Jupiter close to tidal disruption transiting an active F star (2015, background): “Several works showed that hot Jupiters’ radii correlate well with their incident irradiation (see e.g. Demory & Seager 2011, Enoch et al. 2012, or Weiss et al. 2013).”
SOPHIE velocimetry of Kepler transit candidates XVII. The physical properties of giant exoplanets within 400 days of period (2015, background): “To date, very few objects have been characterised independently by both techniques (Weiss et al. 2013; Barros et al. 2014; Bruno et al. 2015).”
UNDERSTANDING THE MASS–RADIUS RELATION FOR SUB-NEPTUNES: RADIUS AS A PROXY FOR COMPOSITION (2013, background): “In recent years this has generated a much fuller understanding of the mass-radius relation, especially for sub-Neptune and super-Earth sized planets (Weiss et al. 2013).”
LOW FALSE POSITIVE RATE OF KEPLER CANDIDATES ESTIMATED FROM A COMBINATION OF SPITZER AND FOLLOW-UP OBSERVATIONS (2015, methodology): “While the radial velocity technique allowed the confirmation of the planetary nature of Kepler-89d (Weiss et al. 2013), Kepler-94b (Marcy et al. 2014), Kepler-102d,e (Marcy et al. 2014).”
The GAPS Programme with HARPS-N at TNG - XIV. Investigating giant planet migration history via improved eccentricity and mass determination for 231 transiting planets (2017, unknown): “1 M Jup in compact multi-planet systems, such as the already mentioned WASP-47 and Kepler-101 systems, but also Kepler-9 (Holman et al. 2010; Borsato et al. 2014) and Kepler-89 (Weiss et al. 2013), were excluded.”
DENSITY AND ECCENTRICITY OF KEPLER PLANETS (2012, unknown): “After the submission of this paper, Weiss et al. (2013) published a related study based on radial velocity data.”
The California-Kepler Survey. V. Peas in a Pod: Planets in a Kepler Multi-planet System Are Similar in Size and Regularly Spaced (2017, unknown): “…precise planet radii to estimates of planet masses (Mp) and densities (ρp) via the empirical mass-radius relationships of Weiss & Marcy (2014) and Weiss et al. (2013): Rp/R⊕ < 1.5 : ρp = 2.43 + 3.39(Rp/R⊕)g cm −3 Mp = (ρp/5.51g cm −3)(Rp/R⊕) 3 M⊕ (6) 1.5 ≤ Rp/R⊕ ≤ 4.0 : Mp = 2.69(Rp/R⊕) 0.93 M⊕…”