  In this paper, we present the details of the ab initio high-precision
configuration interaction and many-body perturbation theory calculations that
were used in a previous work to place limits on the dependence of the
fine-structure constant, alpha, on the gravitational field of the white-dwarf
star G191-B2B. These calculations were combined with laboratory wavelengths and
spectra from the Hubble Space Telescope Imaging Spectrograph to obtain limits
on the gravitational alpha-dependence using Fe V and Ni V transitions. The
uncertainty in these results are dominated by the uncertainty in the laboratory
wavelengths. In this work we also present ab initio calculations of the
isotopic shifts of the Fe V transitions. We show that improved laboratory
spectra will enable determination of the relative isotope abundances in Fe V to
an accuracy ~20%. Therefore this work provides a strong motivation for new
laboratory measurements.
