€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