  To understand giant planet formation, we need to focus on host stars close to
$1.7\ \rm M_{\odot}$, where the occurrence rate of these planets is the
highest. In this initial study, we carry out pebble-driven core accretion
planet formation modelling to investigate the trends and optimal conditions for
the formation of giant planets around host stars in the range of $1{-}2.4\ \rm
M_{\odot}$. We find that giant planets are more likely to form in systems with
a larger initial disk radius; higher disk gas accretion rate; pebbles of $\sim$
millimeter in size; and birth location of the embryo at a moderate radial
distance of $\sim 10$ AU. We also conduct a population synthesis study of our
model and find that the frequency of giant planets and super-Earths decreases
with increasing stellar mass. This contrasts the observational peak at $1.7\
\rm M_{\odot}$, stressing the need for strong assumptions on stellar mass
dependencies in this range. Investigating the combined effect of stellar mass
dependent disk masses, sizes, and lifetimes in the context of planet population
synthesis studies is a promising avenue to alleviate this discrepancy. The
hot-Jupiter occurrence rate in our models is $\sim 0.7{-}0.8\%$ around $1\ \rm
M_{\odot}$ - similar to RV observations around Sun-like stars, but drastically
decreases for higher mass stars.

Earth and Planetary Astrophysics;Solar and Stellar Astrophysics