The influence of general-relativity effects, dynamical tides and collisions on planet-planet scattering close to the star. (arXiv:1904.01420v1 [astro-ph.EP])
<a href="http://arxiv.org/find/astro-ph/1/au:+Marzari_F/0/1/0/all/0/1">F. Marzari</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nagasawa_M/0/1/0/all/0/1">M. Nagasawa</a>

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. 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.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.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. 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.

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. 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.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.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. 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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