  We describe how the accurate characterization of exoplanetary atmospheres in
the ELT and JWST era will inevitably require taking into consideration the
stellar inhomogeneities caused by convection and magnetic fields. The existing
evidence that demonstrates the mixture of stellar and planetary signatures in
observed transiting spectra is presented. Finally, we discuss how to
disentangle these two components through a multipronged approach that includes
new solar reference spectra, improved MHD modeling, and synergistic
collaborations between the communities involved, from solar to stellar and
exoplanet astronomers.
