  With observational efforts moving from the discovery into the
characterisation mode, systematic campaigns that cover large ranges of global
stellar and planetary parameters will be needed. We aim to uncover cloud
formation trends and globally changing chemical regimes due to the host star's
effect on the thermodynamic structure of their atmospheres. We aim to provide
input for exoplanet missions like JWST, PLATO, and Ariel, as well as potential
UV missions ARAGO, PolStar or POLLUX. Pre-calculated 3D GCMs for M, K, G, F
host stars are the input for our kinetic cloud model. Gaseous exoplanets fall
broadly into three classes: i) cool planets with homogeneous cloud coverage,
ii) intermediate temperature planets with asymmetric dayside cloud coverage,
and iii) ultra-hot planets without clouds on the dayside. In class ii),} the
dayside cloud patterns are shaped by the wind flow and irradiation. Surface
gravity and planetary rotation have little effect. Extended atmosphere profiles
suggest the formation of mineral haze in form of metal-oxide clusters (e.g.
(TiO2)_N). The dayside cloud coverage is the tell-tale sign for the different
planetary regimes and their resulting weather and climate appearance. Class (i)
is representative of planets with a very homogeneous cloud particle size and
material compositions across the globe (e.g., HATS-6b, NGTS-1b), classes (ii,
e.g., WASP-43b, HD\,209458b) and (iii, e.g., WASP-121b, WP0137b) have a large
day/night divergence of the cloud properties. The C/O ratio is, hence,
homogeneously affected in class (i), but asymmetrically in class (ii) and
(iii). The atmospheres of class (i) and (ii) planets are little affected by
thermal ionisation, but class (iii) planets exhibit a deep ionosphere on the
dayside. Magnetic coupling will therefore affect different planets differently
and will be more efficient on the more extended, cloud-free dayside.

Earth and Planetary Astrophysics;Solar and Stellar Astrophysics