  We present new models for the forward and reverse shock thermal X-ray
emission from core-collapse and Type Ia supernova remnants (SNRs) which include
the efficient production of cosmic rays via non-linear diffusive shock
acceleration (DSA). Our CR-hydro-NEI code takes into account non-equilibrium
ionization (NEI), hydrodynamic effects of efficient CR production on the SNR
evolution, and collisional temperature equilibration among heavy ions and
electrons in both the shocked supernova (SN) ejecta and the shocked
circumstellar material. While X-ray emission is emphasized here, our code
self-consistently determines both thermal and non-thermal broadband emission
from radio to TeV energies. We include Doppler broadening of the spectral lines
by thermal motions of the ions and by the remnant expansion. We study, in
general terms, the roles which the ambient environment, progenitor models,
temperature equilibration, and processes related to DSA have on the thermal and
non-thermal spectra. The study of X-ray line emission from young SNRs is a
powerful tool for determining specific SN elemental contributions, and for
providing critical information that helps to understand the type and energetics
of the explosion, the composition of the ambient medium in which the SN
exploded, and the ionization and dynamics of the hot plasma in the shocked SN
ejecta and interstellar medium. With the approaching launch of the
next-generation X-ray satellite Astro-H, observations of spectral lines with
unprecedented high resolution will become a reality. Our self-consistent
calculations of the X-ray spectra from various progenitors will help interpret
future observations of SNRs.
