Planet–Planet Gravitational Scattering

Marzari, F.

doi:10.1002/9783527629763.ch11

Cited by 6 publications

(1 citation statement)

References 38 publications

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“…In the decades following 51 Peg b's discovery, a bewildering variety of planets and planetary candidates have been found very close to their host stars, from hot Jupiters like 51 Peg b to hot Neptunes like GJ 1214 b (Charbonneau et al 2009) to hot Earths like Kepler-78 b (Sanchis-Ojeda et al 2013). Early studies suggested these short-period planets formed in orbits 1 AU and arrived near their current orbits through gas disk migration (Armitage & Rice 2005) or dynamical excitation followed by tidal circularization (Marzari 2010). However, which and whether one of these two broad categories dominated the planets' origins remain unclear.…”

Section: Introductionmentioning

confidence: 99%

A New Model of Roche Lobe Overflow for Short-period Gaseous Planets and Binary Stars

Jackson

Arras

Penev

et al. 2017

ApJ

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Some close-in gaseous exoplanets are nearly in Roche lobe contact, and previous studies show that tidal decay can drive hot Jupiters into contact during the main sequence of their host stars. Improving on a previous model, we present a revised model for mass transfer in a semidetached binary system that incorporates an extended atmosphere around the donor and allows for an arbitrary mass ratio. We apply this new formalism to hypothetical, confirmed, and candidate planetary systems to estimate mass-loss rates and compare with models of evaporative mass loss. Overflow may be significant for hot Neptunes out to periods of ∼2 days, while for hot Jupiters, it may only be important inward of 0.5 days. We find that CoRoT-24 b may be losing mass at a rate of more than an Earth mass in a gigayear. The hot Jupiter WASP-12 b may lose an Earth mass in a megayear, while the putative planet PTFO8-8695 orbiting a T Tauri star might shed its atmosphere in a few megayears. We point out that the orbital expansion that can accompany mass transfer may be less effective than previously considered because the gas accreted by the host star removes some of the angular momentum from the orbit, but simple scaling arguments suggest that the Roche lobe overflow might remain stable. Consequently, the recently discovered small planets in ultrashort periods (<1 day) may not be the remnants of hot Jupiters/Neptunes. The new model presented here has been incorporated into Modules for Experiments in Stellar Astrophysics (MESA).

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Section: Introductionmentioning

confidence: 99%

A New Model of Roche Lobe Overflow for Short-period Gaseous Planets and Binary Stars

Jackson

Arras

Penev

et al. 2017

ApJ

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The Role of Interactions Between Stars and Their Planets

Lanza

2022

Demographics of Exoplanetary Systems

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Influence of general-relativity effects, dynamical tides, and collisions on planet–planet scattering close to the star

Marzari

Nagasawa

2019

A&A

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Context. Planet-Planet scattering is an efficient and robust dynamical mechanism for producing eccentric exoplanets. Coupled to tidal interactions with the central star, it can also explain close-in giant planets on circularized and potentially misaligned orbits. Aims. We explore scattering events occurring close to the star and test if they can reproduce the main features of the observed orbital distribution of giant exoplanets on tight orbits. Methods. In our modeling we exploit a numerical integration code based on the Hermite algorithm and including the effects of general relativity, dynamical tides and two-body collisions.Results. We find that P-P scattering events occurring in systems with three giant planets initially moving on circular orbits close to their star produce a population of planets similar to the presently observed one, including eccentric and misaligned close-in planets. The contribution of tides and general relativity is relevant in determining the final outcome of the chaotic phase. Conclusions. Even if two-body collisions dominate the chaotic evolution of three planets in crossing orbits close to their star, the final distribution shows a significant number of planets on eccentric orbits. The highly misaligned close-in giant planets are instead produced by systems where the initial semi-major axis of the inner planet was around 0.2 au or beyond.

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Planet–Planet Gravitational Scattering

Cited by 6 publications

References 38 publications

A New Model of Roche Lobe Overflow for Short-period Gaseous Planets and Binary Stars

A New Model of Roche Lobe Overflow for Short-period Gaseous Planets and Binary Stars

The Role of Interactions Between Stars and Their Planets

Influence of general-relativity effects, dynamical tides, and collisions on planet–planet scattering close to the star

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