Orbital dynamics of exoplanetary systems Kepler-62, HD 200964 and Kepler-11

Mia, Rajib; Kushvah, Badam Singh

doi:10.1093/mnras/stw086

Cited by 31 publications

(9 citation statements)

References 22 publications

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“…Five of the six planets transit their star, but the secondoutermost planet was discovered with the radial velocity technique (Buchhave et al 2016). Kepler-11's and Kepler-20's stellar ages have been estimated at 3.2±0.9 Gyr (Bedell et al 2017) and 7.6±3.7 Gyr (Buchhave et al 2016), respectively, indicating that each system is long-term stable (see also Migaszewski et al 2012;Mahajan & Wu 2014;Hands et al 2014;Mia & Kushvah 2016;Jontof-Hutter et al 2017).…”

Section: Introductionmentioning

confidence: 99%

The origins of nearly coplanar, non-resonant systems of close-in super-Earths

Esteves

Izidoro

Raymond

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Some systems of close-in “super-Earths” contain five or more planets on non-resonant but compact and nearly coplanar orbits. The Kepler-11 system is an iconic representative of this class of system. It is challenging to explain their origins given that planet-disk interactions are thought to be essential to maintain such a high degree of coplanarity, yet these same interactions invariably cause planets to migrate into chains of mean motion resonances. Here we mine a large dataset of dynamical simulations of super-Earth formation by migration. These simulations match the observed period ratio distribution as long as the vast majority of planet pairs in resonance become dynamically unstable. When instabilities take place resonances are broken during a late phase of giant impacts, and typical surviving systems have planet pairs with significant mutual orbital inclinations. However, a subset of our unstable simulations matches the Kepler-11 system in terms of coplanarity, compactness, planet-multiplicity and non-resonant state. This subset have dynamical instability phases typically much shorter than ordinary systems. Unstable systems may keep a high degree of coplanarity post-instability if planets collide at very low orbital inclinations (≲ 1○) or if collisions promote efficient damping of orbital inclinations. If planetary scattering during the instability takes place at low orbital inclinations (i ≲ 1○), orbital inclinations are barely increased by encounters before planets collide.When planetary scattering pumps orbital inclinations to higher values (≳ 1○) planets tend to collide at higher mutual orbital inclinations, but depending on the geometry of collisions mergers’ orbital inclinations may be efficiently damped. Each of these formation pathways can produce analogues to the Kepler-11 system.

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Section: Introductionmentioning

confidence: 99%

The origins of nearly coplanar, non-resonant systems of close-in super-Earths

Esteves

Izidoro

Raymond

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…The residuals between the theoretical velocity and the data are shown in the bottom panel. (Wittenmyer et al 2012), investigated in more detail the resonant behavior exhibited for the reported parameters (Mia & Kushvah 2016) and investigated other, more complex scenarios for the formation of HD 200964 (Emel'yanenko 2012, Tadeu dos Santos et al 2015 4. METHODS In this work, in addition to analyzing a baseline of data longer than that used in JPH11, we investigate the underlying posterior by explicitly conditioning our Markov chain Monte Carlo (MCMC) search on longterm stability.…”

Section: Previous Analysismentioning

confidence: 99%

Measuring the Orbital Parameters of Radial Velocity Systems in Mean-motion Resonance: A Case Study of HD 200964

Rosenthal

Jacobson-Galán

Nelson

et al. 2019

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The presence of mean motion resonances (MMRs) complicates analysis and fitting of planetary systems observed through the radial velocity (RV) technique. MMR can allow planets to remain stable in regions of phase space where strong planet-planet interactions would otherwise destabilize the system. These stable orbits can occupy small phase space volumes, allowing MMRs to strongly constrain system parameters, but making searches for stable orbital parameters challenging. Furthermore, libration of the resonant angle and dynamical interaction between the planets introduces another, long period variation into the observed RV signal, complicating analysis of the periods of the planets in the system. We discuss this phenomenon using the example of HD 200964. By searching through parameter space and numerically integrating each proposed set of planetary parameters to test for long term stability, we find stable solutions in the 7:5 and 3:2 MMRs in addition to the originally identified 4:3 MMR. The 7:5 configuration provides the best match to the data, while the 3:2 configuration provides the most easily understood formation scenario. In reanalysis of the originally published shorter-baseline data, we find fits in both the 4:3 and 3:2 resonances, but not the 7:5. Because the time baseline of the data is less than the resonant libration period, the current best fit to the data may not reflect the actual resonant configuration. In the absence of a full sample of the longer libration period, we find that it is of paramount importance to incorporate long term stability when fitting for the system's orbital configuration.

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“…Few planetary systems are discovered containing at least one earth like planet where life can exist. For example Kepler-62 (Borucki et al, 2013;Mia and Kushvah, 2016a), Kepler-186 (Bolmont et al, 2014), Kepler-69 (Barclay et al, 2013) and HD 40307 (Tuomi et al, 2013) systems consist at least one earth like planet in the habitable zone. Among about 5000 newly discovered exoplanetary systems only few systems found in mean motion resonances(MMRs).…”

Section: Introductionmentioning

confidence: 99%

Analysis of the dynamics of the resonant planetary system HD 45364

Mia

Paul

2022

Preprint

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The aim of this work is to analyse the orbital dynamics and stability of exoplanetary system in which two planets are in nearly 3:2 MMR. We have taken HD 45364 system for our study in which two planets are most likely in a 3:2 MMR. We have plotted two resonant angles and the relative apsidal longitudes and it is observed that they are librating around a constant value. From this observation our opinion is that there exist nearly 3:2 MMR between HD 45364b and HD 45364c. The perturbative solution is obtained for the time variation of the semi-major axes. The short and long term variations of semimajor axes are studied. For the validation of our analytical results we have compared our analytical solutions with the numerical solutions. The effect of planetary perturbations on eccentricity is studied with the help of secular resonance dynamics theory. The short and long term variations of eccentricities of HD 45364b and HD 45364c are shown graphically. Moreover, using the latest stability criteria, we have studied the dynamical stability of HD 45364 system.

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Orbital dynamics of exoplanetary systems Kepler-62, HD 200964 and Kepler-11

Cited by 31 publications

References 22 publications

The origins of nearly coplanar, non-resonant systems of close-in super-Earths

The origins of nearly coplanar, non-resonant systems of close-in super-Earths

Measuring the Orbital Parameters of Radial Velocity Systems in Mean-motion Resonance: A Case Study of HD 200964

Analysis of the dynamics of the resonant planetary system HD 45364

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