Response to Langlois <i>et al</i> (LE 01059)

Thorne, Kym; Bowen, Derrick John; McCune, C. Anne; Worwood, Mark

doi:10.1046/j.1365-2141.2003.04798.x

Cited by 52 publications

(79 citation statements)

References 4 publications

(8 reference statements)

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“…The strongest detections of dense exoplanets, mostly in RV but also including Kepler-36 b (Carter et al 2012), indicate primarily rocky compositions for planets up to ≈1.6 R ⊕ in size (Dressing et al 2015). However, strong mass upper limits on the weaker detections of slightly larger planets include several low-mass planets that are too low in bulk density to be rocky (e.g., Kepler-11 b and Kepler-11 f;Lissauer et al 2013).…”

Section: Introductionmentioning

confidence: 99%

“…However, the sensitivity of TTV to low-mass planets beyond the range of RV has enabled the characterization of volatile-rich planets that are far enough from their hosts to have avoided significant mass loss. The precise TTV mass detections to date show a remarkablediversity in planetary density in the mass range from 2 to 8 M ⊕ (Lissauer et al 2011a;Carter et al 2012;Jontof-Hutter et al 2014;Masuda 2014;Ofir et al 2014).…”

Section: Introductionmentioning

confidence: 99%

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SECURE MASS MEASUREMENTS FROM TRANSIT TIMING: 10 KEPLER EXOPLANETS BETWEEN 3 AND 8 M _⊕ WITH DIVERSE DENSITIES AND INCIDENT FLUXES

Jontof-Hutter

Ford

Rowe

et al. 2016

ApJ

176

147

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We infer dynamical masses in eight multiplanet systems using transit times measured from Keplerʼs complete dataset, including short-cadence data where available. Of the 18dynamical masses that we infer, 10pass multiple tests for robustness. These are in systemsKepler-26 (KOI-250), Kepler-29 (KOI-738), Kepler-60 (KOI-2086), , and Kepler-307 (KOI-1576). Kepler-105 c has a radius of 1.3 R ⊕ and a density consistent with an Earth-like composition. Strong transit timing variation(TTV) signals were detected from additional planets, but their inferred masses were sensitive to outliers or consistent solutions could not be found with independently measured transit times, including planets orbitingKepler-49 (KOI-248), Kepler-57 (KOI-1270), Kepler-105 (KOI-115), and Kepler-177 (KOI-523). Nonetheless, strong upper limits on the mass of Kepler-177 c imply an extremely low density of∼0.1 g cm −3 . In most cases, individual orbital eccentricities were poorly constrained owingto degeneracies in TTV inversion. For five planet pairs in our sample, strong secular interactions imply a moderatetohigh likelihood of apsidal alignment over a wide range of possible eccentricities. We also find solutions for the three planets known to orbit Kepler-60 in a Laplace-like resonance chain. However, nonlibrating solutions also match the transittiming data. For six systems, we calculate more precise stellar parameters than previously known, enabling useful constraints on planetary densities where we have secure mass measurements. Placing these exoplanets on the mass-radius diagram, we find thata wide range of densities isobserved among sub-Neptune-mass planets and that the range in observed densities is anticorrelated with incident flux.

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

SECURE MASS MEASUREMENTS FROM TRANSIT TIMING: 10 KEPLER EXOPLANETS BETWEEN 3 AND 8 M _⊕ WITH DIVERSE DENSITIES AND INCIDENT FLUXES

Jontof-Hutter

Ford

Rowe

et al. 2016

ApJ

176

147

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“…Transit timing variations (TTVs; Miralda-Escudé 2002; Agol et al 2005;Holman & Murray 2005) have proved useful for constraining the masses and orbital elements of exoplanets (e.g., Carter et al 2012;Huber et al 2013;Nesvorný et al 2013). To date, most TTV studies have focused on pairs of planets near mean motion resonances (MMRs) and in particular on those near first-order resonances.…”

Section: Introductionmentioning

confidence: 99%

Transit Timing Variations for Planets Near Eccentricity-Type Mean Motion Resonances

Deck

Agol

2016

ApJ

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We derive the transit timing variations (TTVs) of two planets near a second-order mean motion resonance (MMR) on nearly circular orbits. We show that the TTVs of each planet are given by sinusoids with a frequency of --jn j n 2 2 1 ( ) , where  j 3 is an integer characterizing the resonance and n 2 and n 1 are the mean motions of the outer and inner planets, respectively. The amplitude of the TTV depends on the mass of the perturbing planet, relative to the mass of the star, and on both the eccentricities and longitudes of pericenter of each planet. The TTVs of the two planets are approximated anti-correlated, with phases of f and f p » + , where the phase f also depends on the eccentricities and longitudes of pericenter. Therefore, the TTVs caused by proximity to a second-order MMR do not in general uniquely determine both planet masses, eccentricities, and pericenters. This is completely analogous to the case of TTVs induced by two planets near a first-order MMR. We explore how other TTV signals, such as the short-period synodic TTV or a first-order resonant TTV, in combination with the second-order resonant TTV, can break degeneracies. Finally, we derive approximate formulae for the TTVs of planets near any order eccentricity-type MMR; this shows that the same basic sinusoidal TTV structure holds for all eccentricity-type resonances. Our general formula reduces to previously derived results near first-order MMRs.

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“…Among the many interesting systems identified by this mission is Kepler-36, which has two planets orbiting near the 7:6 mean motion resonance (MMR; Carter et al 2012). These two planets have orbital periods of 13.8 and 16.2 days, have masses of 4.5 and 8.1 M ⊕ , and have radii of 1.5 and 3.7 R ⊕ for the inner and outer planets, respectively.…”

Section: Introductionmentioning

confidence: 99%

Dynamical Considerations for Life in Multi-Habitable Planetary Systems

Steffen

2016

ApJ

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Inspired by the close-proximity pair of planets in the Kepler-36 system, we consider two effects that may have important ramifications for the development of life in similar systems where a pair of planets may reside entirely in the habitable zone of the hosting star. Specifically, we run numerical simulations to determine whether strong, resonant (or non-resonant) planet-planet interactions can cause large variations in planet obliquity-thereby inducing large variations in climate. We also determine whether or not resonant interactions affect the rate of lithopanspermia between the planet pair-which could facilitate the growth and maintenance of life on both planets. We find that first-order resonances do not cause larger obliquity variations when compared with nonresonant cases. We also find that these resonant interactions are not a primary consideration in lithopanspermia. Lithopanspermia is enhanced significantly as the planet orbits come closer together-reaching nearly the same rate as ejected material falling back to the surface of the originating planet (assuming that the ejected material makes it out to the location of our initial conditions). Thus, in both cases our results indicate that close-proximity planet pairs in multi-habitable systems are conducive to life in the system.

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Response to Langlois et al (LE 01059)

Cited by 52 publications

References 4 publications

SECURE MASS MEASUREMENTS FROM TRANSIT TIMING: 10 KEPLER EXOPLANETS BETWEEN 3 AND 8 M _⊕ WITH DIVERSE DENSITIES AND INCIDENT FLUXES

SECURE MASS MEASUREMENTS FROM TRANSIT TIMING: 10 KEPLER EXOPLANETS BETWEEN 3 AND 8 M _⊕ WITH DIVERSE DENSITIES AND INCIDENT FLUXES

Transit Timing Variations for Planets Near Eccentricity-Type Mean Motion Resonances

Dynamical Considerations for Life in Multi-Habitable Planetary Systems

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Response to Langlois et al (LE 01059)

Cited by 52 publications

References 4 publications

SECURE MASS MEASUREMENTS FROM TRANSIT TIMING: 10 KEPLER EXOPLANETS BETWEEN 3 AND 8 M ⊕ WITH DIVERSE DENSITIES AND INCIDENT FLUXES

SECURE MASS MEASUREMENTS FROM TRANSIT TIMING: 10 KEPLER EXOPLANETS BETWEEN 3 AND 8 M ⊕ WITH DIVERSE DENSITIES AND INCIDENT FLUXES

Transit Timing Variations for Planets Near Eccentricity-Type Mean Motion Resonances

Dynamical Considerations for Life in Multi-Habitable Planetary Systems

Contact Info

Product

Resources

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SECURE MASS MEASUREMENTS FROM TRANSIT TIMING: 10 KEPLER EXOPLANETS BETWEEN 3 AND 8 M _⊕ WITH DIVERSE DENSITIES AND INCIDENT FLUXES

SECURE MASS MEASUREMENTS FROM TRANSIT TIMING: 10 KEPLER EXOPLANETS BETWEEN 3 AND 8 M _⊕ WITH DIVERSE DENSITIES AND INCIDENT FLUXES