  Stellar inclination is an important parameter for many astrophysical studies.
Although different techniques allow us to estimate stellar inclinationt for
fast rotators, it becomes much more difficult when stars are rotating slower
than $\sim2$-2.5 \kms. By using the new activity simulation SOAP 2.0 that can
reproduce the photometric and spectroscopic variations induced by stellar
activity, we are able to fit observations of solar-type stars and derive their
inclination. For HD189733, we estimate the stellar inclination to be
$i=84^{+6}_{-20}$ degrees, which implies a star-planet obliquity of
$\psi=4^{+18}_{-4}$ considering previous measurements of the spin-orbit angle.
For $\alpha$ Cen B, we derive an inclination of $i=45^{+9}_{-19}$, which
implies that the rotational spin of the star is not aligned with the orbital
spin of the $\alpha$ Cen binary system. In addition, assuming that $\alpha$ Cen
Bb is aligned with its host star, no transit would occur. The inclination of
$\alpha$ Cen B can be measured using 40 radial-velocity measurements, which is
remarkable given that the projected rotational velocity of the star is smaller
than $1.15\,km\,s^{-1}$.
