  The search for satellites around exoplanets represents one of the greatest
challenges in advancing the characterization of planetary systems. Currently,
we can only detect massive satellites, which resemble additional planetary
companions rather than rocky moons. It is not yet well understood whether such
substellar pairs, known as binary planets, are common or how they form. In this
study, we investigated the formation scenario for binary planets resulting from
tidal dissipation during close encounters in the gravitational instability
scenario. We conducted seven sets of simulations, varying the number of initial
planets injected into the system from two to five, as well as the amount of
energy lost due to tides. Our results demonstrate that this formation mechanism
is quite efficient in producing binary planets, with an average occurrence rate
for the simulated systems of 14.3%. Additionally, we present the distribution
of relevant physical parameters (semi-major axis, eccentricity, mass ratios,
and formation time) for planet-planet pairs. We also provide comprehensive
statistics for single planets and planet-planet pairs.
