  Determining the behaviour of convection and clouds is one of the biggest
challenges in our understanding of exoplanetary climates. Given the lack of in
situ observations, one of the most preferable approaches is to use
cloud-resolving or cloud-permitting models (CPM). Here we present CPM
simulations in a quasi-global domain with high spatial resolution (4$\times$4
km grid) and explicit convection to study the cloud regime of 1 to 1 tidally
locked rocky planets orbiting around low-mass stars. We show that the
substellar region is covered by deep convective clouds and cloud albedo
increases with increasing stellar flux. The CPM produces relatively less cloud
liquid water concentration, smaller cloud coverage, lower cloud albedo, and
deeper H2O spectral features than previous general circulation model (GCM)
simulations employing empirical convection and cloud parameterizations.
Furthermore, cloud streets--long bands of low-level clouds oriented nearly
parallel to the direction of the mean boundary-layer winds--appear in the CPM
and substantially affect energy balance and surface precipitation at a local
level.
