  Stellar activity induced by active structures (eg, spots, faculae) is known
to strongly impact the radial velocity time series. It then limits the
detection of small planetary RV signals (eg, an Earth-mass planet in the
habitable zone of a solar-like star). In previous papers, we studied the
detectability of such planets around the Sun seen as an edge-on star. For that
purpose, we computed the RV and photometric variations induced by solar
magnetic activity, using all active structures observed over one entire cycle.
Our goal is to perform similar studies on stars with different physical and
geometrical properties. As a first step, we focus on Sun-like stars seen with
various inclinations, and on estimating detection capabilities with forthcoming
instruments. To do so, we first parameterize the solar active structures with
the most realistic pattern so as to obtain results consistent with the observed
ones. We simulate the growth, evolution and decay of solar spots, faculae and
network, using parameters and empiric laws derived from solar observations and
literature. We generate the corresponding structure lists over a full solar
cycle. We then build the resulting spectra and deduce the RV and photometric
variations for a `Sun' seen with various inclinations. The produced RV signal
takes into account the photometric contribution of structures as well as the
attenuation of the convective blueshift. The comparison between our simulated
activity pattern and the observed one validates our model. We show that the
inclination of the stellar rotation axis has a significant impact on the time
series. RV long-term amplitudes as well as short-term jitters are significantly
reduced when going from edge-on to pole-on configurations. Assuming spin-orbit
alignment, the optimal configuration for planet detection is an inclined star
(i~45{\deg}).
