€Many aspects deserve further investigation: here are some
–boundary layer in non-magnetics
–the base of the post-shock accretion flow in magnetics
and the way this diffuses into
the white dwarf
–heating of the atmosphere around the accretion
region in magnetics, and effect on overall energy
distribution
–low accretion rate regimes in magnetics, whether
this results in a bombardment
solution (no shock)
–disk-magnetosphere interaction in IPs: important in a
number of contexts
–disk-stream interactions in non-magnetics
–magnetosphere-stream interactions in Polars
–irradiation of the stream and secondary by X-ray flux
–more astrophysics in the post-shock flow models
(such as the separation of electron and ion fluids)
€Combinations of high quality data (eg. eclipse mapping of spectra) and new astrophysical fluid computations will transform the field and allow ever more intricate understandings of accretion phenomena to be achieved