# The influence of general-relativity effects, dynamical tides and collisions on planet-planet scattering close to the star

## TL;DR

This study investigates how planet-planet scattering near the star, including effects of general relativity, tides, and collisions, can produce the observed distribution of close-in eccentric and misaligned giant exoplanets.

## Contribution

It demonstrates that scattering events with these effects can reproduce observed exoplanet orbital features, highlighting the importance of general relativity and tides.

## Key findings

- Scattering near the star can produce eccentric and misaligned close-in planets.
- Tides and general relativity significantly influence the final orbital configurations.
- Collisions dominate the chaotic evolution but still result in eccentric orbits.

## Abstract

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.