  The detection of Earth-size exoplanets is a technological and data analysis
challenge. Future progress in Earth-mass exoplanet detection is expected from
the development of extreme precision radial velocity measurements. Increasing
radial velocity precision requires developing a new physics-based data analysis
methodology to discriminate planetary signals from host-star-related effects,
taking stellar variability and instrumental uncertainties into account. In this
work, we investigate and quantify stellar disturbances of the planet-hosting
solar-type star HD121504 from 3D radiative modeling obtained with the
StellarBox code. The model has been used for determining statistical properties
of the turbulent plasma and obtaining synthetic spectroscopic observations for
several Fe I lines at different locations on the stellar disk to mimic
high-resolution spectroscopic observations.
