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 \sim 2 -2.5 km s ^ { -1 } . 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 } .