  A perturbative analysis is used to investigate the effect of rotation on the
instability of a steady accretion shock (SASI) in a simple toy-model, in view
of better understanding supernova explosions in which the collapsing core
contains angular momentum. A cylindrical geometry is chosen for the sake of
simplicity. Even when the centrifugal force is very small, rotation can have a
strong effect on the non axisymmetric modes of SASI by increasing the growth
rate of the spiral modes rotating in the same direction as the steady flow.
Counter-rotating spiral modes are significantly damped, while axisymmetric
modes are hardly affected by rotation. The growth rates of spiral modes have a
nearly linear dependence on the specific angular momentum of the flow. The
fundamental one-armed spiral mode (m=1) is favoured for small rotation rates,
whereas stronger rotation rates favour the mode m=2. A WKB analysis of higher
harmonics indicates that the efficiency of the advective-acoustic cycles
associated to spiral modes is strongly affected by rotation in the same manner
as low frequency modes, whereas the purely acoustic cycles are stable. These
results suggest that the linear phase of SASI in rotating core-collapse
supernovae naturally selects a spiral mode rotating in the same direction of
the flow, as observed in the 3D numerical simulations of Blondin & Mezzacappa
(2007). This emphasizes the need for a 3D approach of rotating core-collapse,
before conclusions on the explosion mechanisms and pulsar kicks can be drawn.
