  Stellar activity is the main limitation to the detection of Earth-twins using
the RV technique. Despite many efforts in trying to mitigate the effect of
stellar activity using empirical and statistical techniques, it seems that we
are facing an obstacle that will be extremely difficult to overcome using
current techniques. In this paper, we investigate a novel approach to derive
precise RVs considering the wealth of information present in high-resolution
spectra. This new method consists in building a master spectrum from all
observations and measure the RVs of each spectral line in a spectrum relative
to it. When analysing several spectra, the final product is the RVs of each
line as a function of time. We demonstrate on three stars intensively observed
with HARPS that our new method gives RVs that are extremely similar to the ones
derived from the HARPS data reduction software. Our new approach to derive RVs
demonstrates that the non-stability of daily HARPS wavelength solution induces
night-to-night RV offsets with an standard deviation of 0.4 m/s, and we propose
a solution to correct for this systematic. Finally, and this is probably the
most astrophysically relevant result of this paper, we demonstrate that some
spectral lines are strongly affected by stellar activity while others are not.
By measuring the RVs on two carefully selected subsample of spectral lines, we
demonstrate that we can boost by a factor of 2 or mitigate by a factor of 1.6
the red noise induced by stellar activity in the 2010 RVs of Alpha Cen B. By
measuring the RVs of each spectral line, we are able to reach the same RV
precision as other approved techniques. In addition, this new approach allows
to demonstrate that each line is differently affected by stellar activity.
Preliminary results show that studying in details the behaviour of each
spectral line is probably the key to overcome stellar activity.
