A resonant chain of four transiting, sub-Neptune planets

Mills, Sean M.; Fabrycky, Daniel C.; Migaszewski, Cezary; Ford, Eric B.; Petigura, Erik A.; Isaacson, Howard

doi:10.1038/nature17445

Cited by 220 publications

(277 citation statements)

References 50 publications

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“…Kepler-223/KOI-730 is a four-planet system that also has two interlocking three-body resonances studied extensively by Mills et al (2016). Its planets are in two-body resonances with each other forming a multiresonant chain that also supports the three and fourbody commensurabilities seen in Kepler-80.…”

Section: 3mentioning

confidence: 99%

A Dynamical Analysis of the Kepler-80 System of Five Transiting Planets

MacDonald

Ragozzine

Fabrycky

et al. 2016

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Kepler has discovered hundreds of systems with multiple transiting exoplanets which hold tremendous potential both individually and collectively for understanding the formation and evolution of planetary systems. Many of these systems consist of multiple small planets with periods less than ∼50 days known as Systems with Tightly-spaced Inner Planets, or STIPs. One especially intriguing STIP, Kepler-80 (KOI-500), contains five transiting planets: f, d, e, b, and c with periods of 1.0, 3.1, 4.6, 7.1, 9.5 days, respectively. We provide measurements of transit times and a transit timing variation (TTV) dynamical analysis. We find that TTVs cannot reliably detect eccentricities for this system, though mass estimates are not affected. Restricting the eccentricity to a reasonable range, we infer masses for the outer four planets (d, e, b, and c) to be 6.75 −0.86 Earth masses, respectively. The similar masses but different radii are consistent with terrestrial compositions for d and e and ∼2% H/He envelopes for b and c. We confirm that the outer four planets are in a rare dynamical configuration with four interconnected three-body resonances that are librating with few degree amplitudes. We present a formation model that can reproduce the observed configuration by starting with a multi-resonant chain and introducing dissipation. Overall, the information-rich Kepler-80 planets provide an important perspective into exoplanetary systems.

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Section: 3mentioning

confidence: 99%

A Dynamical Analysis of the Kepler-80 System of Five Transiting Planets

MacDonald

Ragozzine

Fabrycky

et al. 2016

Self Cite

134

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“…First, although the orbital period we found makes it extremely likely that this newly discovered planet is the outer link in a chain of three-body resonances, the system requires further dynamical analysis to confirm the resonant state. Even though its low S/N will make it difficult, it could be worthwhile to search for Kepler80g's TTVs, perhaps by measuring the timing of many transits averaged together (e.g., Mills et al 2016). Finally, it will be important to assess the impact of a new planet in the resonant chain on the Kepler-80 TTV mass measurements made by MacDonald et al (2016).…”

Section: Newly Validated Planetsmentioning

confidence: 99%

Identifying Exoplanets with Deep Learning: A Five-planet Resonant Chain around Kepler-80 and an Eighth Planet around Kepler-90

2018

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NASA's Kepler Space Telescope was designed to determine the frequency of Earth-sized planets orbiting Sun-like stars, but these planets are on the very edge of the mission's detection sensitivity. Accurately determining the occurrence rate of these planets will require automatically and accurately assessing the likelihood that individual candidates are indeed planets, even at low signal-to-noise ratios. We present a method for classifying potential planet signals using deep learning, a class of machine learning algorithms that have recently become state-of-theart in a wide variety of tasks. We train a deep convolutional neural network to predict whether a given signal is a transiting exoplanet or a false positive caused by astrophysical or instrumental phenomena. Our model is highly effective at ranking individual candidates by the likelihood that they are indeed planets: 98.8% of the time it ranks plausible planet signals higher than false-positive signals in our test set. We apply our model to a new set of candidate signals that we identified in a search of known Kepler multi-planet systems. We statistically validate two new planets that are identified with high confidence by our model. One of these planets is part of a five-planet resonant chain around Kepler-80, with an orbital period closely matching the prediction by three-body Laplace relations. The other planet orbits Kepler-90, a star that was previously known to host seven transiting planets. Our discovery of an eighth planet brings Kepler-90 into a tie with our Sun as the star known to host the most planets.

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“…They recovered a surface density up to ≈5 times that of the MMSN which would allow planets to accrete in situ. However, there is dynamical evidence for planet migration in the Solar System (e.g., Malhotra 1993;Fernández & Ip 1996;Levison et al 2008) and other systems (Lin et al 1996;Mills et al 2016), which would have redistributed mass. Desch (2007) included the migration of the giant planets described by the "Nice" model to derive a steeper power-law profile for the MMSN.…”

Section: Introductionmentioning

confidence: 99%

A minimum mass nebula for M dwarfs

Gaidos

2017

Monthly Notices of the Royal Astronomical Society: Letters

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Recently revealed differences in planets around M dwarf vs. solar-type stars could arise from differences in their primordial disks, and surveys of T Tauri stars find a correlation between stellar mass and disk mass. "Minimum" disks have been reconstructed for the Solar System and solar-type stars and here this exercise is performed for M dwarfs using Kepler-detected planets. Distribution of planet mass between current orbits produces a disk with total mass of ≈0.009M ⊙ and a power-law profile with index α = 2.2. Disk reconstruction from the output of a forward model of planet formation indicates that the effect of detection bias on disk profile is slight and that the observed scatter in planet masses and semi-major axes is consistent with a universal disk profile. This nominal M dwarf disk is more centrally concentrated than those inferred around the solar-type stars observed by Kepler, and the mass surface density beyond 0.02 AU is sufficient for in situ accretion of planets as single embryos. The mass of refractory solids within 0.5 AU is 5.6M ⊕ compared to 4M ⊕ for solar-type stars, in contrast with the trend with total disk mass. The total solids beyond 0.5 AU is sufficient for the core of at least one giant planet.

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A resonant chain of four transiting, sub-Neptune planets

Cited by 220 publications

References 50 publications

A Dynamical Analysis of the Kepler-80 System of Five Transiting Planets

A Dynamical Analysis of the Kepler-80 System of Five Transiting Planets

Identifying Exoplanets with Deep Learning: A Five-planet Resonant Chain around Kepler-80 and an Eighth Planet around Kepler-90

A minimum mass nebula for M dwarfs

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