  Strong magnetic fields in the cores of stars are expected to significantly
modify the behavior of gravity waves: this is likely the origin of suppressed
dipole modes observed in many red giants. However, a detailed understanding of
how such fields alter the spectrum and spatial structure of magnetogravity
waves has been elusive. For a dipole field, we analytically characterize the
horizontal eigenfunctions of magnetogravity modes, assuming that the wavevector
is primarily radial. For axisymmetric modes ($m=0$), the magnetogravity wave
eigenfunctions become Hough functions, and they have a radial turning point for
sufficiently strong magnetic fields. For non-axisymmetric modes ($m\neq0$), the
interaction between the discrete $g$ mode spectrum and a continuum of Alfv\'en
waves produces nearly discontinuous features in the fluid displacements at
critical latitudes associated with a singularity in the fluid equations.
effects. We find that magnetogravity modes cannot propagate in regions with
sufficiently strong magnetic fields, instead becoming evanescent. When
encountering strong magnetic fields, ingoing gravity waves are likely refracted
into outgoing slow magnetic waves. These outgoing waves approach infinite
radial wavenumbers, which are likely to be damped efficiently. However, it may
be possible for a small fraction of the wave power to escape the stellar core
as pure Alfv\'en waves or magnetogravity waves confined to a very narrow
equatorial band. The artificially sharp features in the WKB-separated solutions
suggest the need for global mode solutions which include small terms neglected
in our analysis.
