  To detect Earth-mass planets using the Doppler method, a major obstacle is to
differentiate the planetary signal from intrinsic stellar variability (e.g.,
pulsations, granulation, spots and plages). Convective blueshift, which results
from small-scale convection at the surface of Sun-like stars, is relevant for
Earth-twin detections as it exhibits Doppler noise on the order of 1 m/s. Here,
we present a simple model for convective blueshift based on fundamental
equations of stellar structure. Our model successfully matches observations of
convective blueshift for FGK stars. Based on our model, we also compute the
intrinsic noise floor for stellar granulation in the radial velocity
observations. We find that for a given mass range, stars with higher
metallicities display lower radial-velocity dispersion due to granulation, in
agreement with MHD simulations. We also provide a set of formulae to predict
the amplitude of radial-velocity dispersion due to granulation as a function of
stellar parameters. Our work is vital in identifying the most amenable stellar
targets for EPRV surveys and radial velocity follow-up programmes for TESS,
CHEOPS, and the upcoming PLATO mission.
