To understand giant planet formation, we need to focus on host stars close to
1.7 M⊙​, 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 M⊙​. 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 ∼
millimeter in size; and birth location of the embryo at a moderate radial
distance of ∼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 $1.7\
\rm M_{\odot},stressingtheneedforstrongassumptionsonstellarmassdependenciesinthisrange.Investigatingthecombinedeffectofstellarmassdependentdiskmasses,sizes,andlifetimesinthecontextofplanetpopulationsynthesisstudiesisapromisingavenuetoalleviatethisdiscrepancy.Thehot−Jupiteroccurrencerateinourmodelsis\sim 0.7{-}0.8\%around1\ \rm
M_{\odot}$ - similar to RV observations around Sun-like stars, but drastically
decreases for higher mass stars.Comment: 21 pages, 11 figure