  Shocks, turbulence and winds all influence the electron velocity distribution
in hot plasmas, exciting lower-energy electrons and generating a high-energy
(typically power-law) tail. This effect, typically described as a kappa
distribution can affect both the line and continuum X-ray spectrum emitted by
the plasma. Hahn & Savin (2015) proposed a "Maxwellian decomposition" to
generate the rate coefficients of kappa distributions. Using their method and
the AtomDB atomic database, we have developed a general model to calculate the
emission from a plasma with a kappa distribution. We compare our kappa results
for the charge state distribution and spectra of oxygen to those from KAPPA
package with the ion data available within the CHIANTI atomic database.
Sufficiently energetic electrons, created either in a kappa distribution or
merely a very hot Maxwellian plasma, can also emit via electron-electron (e-e)
bremsstrahlung, a process not previously included in AtomDB. We have added this
process to AtomDB and apply it to calculate the temperature gradients, as well
as the total spectra from the post-shock regions of an accreting magnetic
cataclysmic variable (CV). We find the contribution of e-e bremsstrahlung to
the total spectra exceeds 10% at KT\sim 100 keV, with the total emissivity in
the post-shock accretion stream differing by more than 10% at energies above 60
keV.
