A linear distribution of orbits in compact planetary systems?

Migaszewski, Cezary; Goździewski, Krzysztof; Słonina, Mariusz

doi:10.1093/mnrasl/slt105

Cited by 24 publications

(3 citation statements)

References 28 publications

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“…The migration mechanism and resonance trapping is likely responsible, although in quite smaller scale when concerning the orbits and planetary masses, for creating multiple systems of super-Earth planets discovered by the KEPLER mission (Borucki & Koch 2011;Batalha 2013). A significant sample of KEPLER systems involving four and more planets are found very close to multiple MMRs which might be also explained by a common, inward migration (Migaszewski et al 2013, and references therein).…”

Section: Discussionmentioning

confidence: 94%

Multiple mean motion resonances in the HR 8799 planetary system

Goździewski

Migaszewski

2014

Monthly Notices of the Royal Astronomical Society

115

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HR 8799 is a nearby star hosting at least four ∼ 10 m Jup planets in wide orbits up to ∼ 70 au, detected through the direct, high-contrast infrared imaging. Large companions and debris disks reported interior to ∼ 10 au, and exterior to ∼ 100 au indicate massive protoplanetary disc in the past. The dynamical state of the HR 8799 system is not yet fully resolved, due to limited astrometric data covering tiny orbital arcs. We construct a new, orbital model of the HR 8799 system, assuming rapid migration of the planets after their formation in wider orbits. We found that the HR 8799 planets are likely involved in double Laplace resonance, 1e:2d:4c:8b MMR. Quasi-circular planetary orbits are coplanar with the stellar equator and inclined by ∼ 25 • to the sky plane. This best-fit orbital configuration matches astrometry, debris disk models, and mass estimates from cooling models. The multiple MMR is stable for the age of the star ∼ 160 Myr, for at least 1 Gyr unless significant perturbations to the N-body dynamics are present. We predict four configurations with the fifth hypothetical innermost planet HR 8799f in ∼ 9.7 au, or ∼ 7.5 au orbit, extending the MMR chain to triple Laplace resonance 1f:2e:4d:8c:16b MMR or to the 1f:3e:6d:12c:24b MMR, respectively. Our findings may establish strong boundary conditions for the system formation and its early history.

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Section: Discussionmentioning

confidence: 94%

Multiple mean motion resonances in the HR 8799 planetary system

Goździewski

Migaszewski

2014

Monthly Notices of the Royal Astronomical Society

115

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“…Dissipative dynamics are thought to drive planets into resonant configurations; subsequent planet-planet scattering or stochastic migration forces can randomize the period ratios. Thus, the ratio of Kepler orbital periods in exoplanetary systems is a critical test of planet formation theories (e.g., Rein 2012;Migaszewski et al 2013 Kepler has provided enormous insight into the exoplanetary period ratio distribution. First, Kepler has identified an order of magnitude more planetary systems to date than all other methods and observations combined.…”

Section: Application To Period Ratio Distribution Ofmentioning

confidence: 99%

Efficient Geometric Probabilities of Multi-Transiting Exoplanetary Systems From Corbits

Brakensiek

Ragozzine

2016

ApJ

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NASA's Kepler Space Telescope has successfully discovered thousands of exoplanet candidates using the transit method, including hundreds of stars with multiple transiting planets. In order to estimate the frequency of these valuable systems, it is essential to account for the unique geometric probabilities of detecting multiple transiting extrasolar planets around the same parent star. In order to improve on previous studies that used numerical methods, we have constructed an efficient, semi-analytical algorithm called CORBITS which, given a collection of conjectured exoplanets orbiting a star, computes the probability that any particular group of exoplanets can be observed to transit. The algorithm applies theorems of elementary differential geometry to compute the areas bounded by circular curves on the surface of a sphere (see Ragozzine & Holman 2010). The implemented algorithm is more accurate and orders of magnitude faster than previous algorithms, based on comparisons with Monte Carlo simulations. We use CORBITS to show that the present solar system would only show a maximum of 3 transiting planets, but that this varies over time due to dynamical evolution. We also used CORBITS to geometrically debias the period ratio and mutual Hill sphere distributions of Kepler 's multi-transiting planet candidates, which results in shifting these distributions towards slightly larger values. In an Appendix, we present additional semi-analytical methods for determining the frequency of exoplanet mutual events, i.e., the geometric probability that two planets will transit each other (Planet-Planet Occultation, relevant to transiting circumbinary planets) and the probability that this transit occurs simultaneously as they transit their star. The CORBITS algorithms and several worked examples are publicly available at https://github.com/jbrakensiek/CORBITS.

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“…The Kepler-11 system (Lissauer et al 2011) is a system with six transiting planets. A full dynamical analysis has been carried out for this system, giving constraints on the masses of all planets (Migaszewski et al 2013;Lissauer et al 2013). Several of the planets, despite being only a few Earth masses, have low densities which require H/He atmospheres; this result is puzzling in light of core-accretion theory, which would not predict planets so low in mass to accumulate substantial gaseous envelopes.…”

Section: Kepler 11d/ementioning

confidence: 99%

Measurement of Planet Masses With Transit Timing Variations Due to Synodic “Chopping” Effects

Deck

Agol

2015

ApJ

108

111

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Gravitational interactions between planets in transiting exoplanetary systems lead to variations in the times of transit that are diagnostic of the planetary masses and the dynamical state of the system. Here we show that synodic "chopping" contributions to these transit timing variations (TTVs) can be used to uniquely measure the masses of planets without full dynamical analyses involving direct integration of the equations of motion. We present simple analytic formulae for the chopping signal, which are valid (generally < 10% error) for modest eccentricities e 0.1. Importantly, these formulae primarily depend on the mass of the perturbing planet, and therefore the chopping signal can be used to break the mass/free-eccentricity degeneracy which can appear for systems near first order mean motion resonances. Using a harmonic analysis, we apply these TTV formulae to a number of Kepler systems which had been previously analyzed with full dynamical analyses. We show that when chopping is measured, the masses of both planets can be determined uniquely, in agreement with previous results, but without the need for numerical orbit integrations. This demonstrates how mass measurements from TTVs may primarily arise from an observable chopping signal. The formula for chopping can also be used to predict the number of transits and timing precision required for future observations, such as those made by TESS or PLATO, in order to infer planetary masses through analysis of TTVs. Subject headings: planetary systems 2 Degeneracies have also been identified between eccentricity vector components and between planetary mass and mutual inclination Carter et al. 2012;Huber et al. 2013).3 The short-timescale variations occur on harmonics of the synodic timescale, (P −1 1 − P −1 2 ) −1 , but can sometimes appear to vary on a longer timescale due to aliasing.

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A linear distribution of orbits in compact planetary systems?

Cited by 24 publications

References 28 publications

Multiple mean motion resonances in the HR 8799 planetary system

Multiple mean motion resonances in the HR 8799 planetary system

Efficient Geometric Probabilities of Multi-Transiting Exoplanetary Systems From Corbits

Measurement of Planet Masses With Transit Timing Variations Due to Synodic “Chopping” Effects

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