We present new models for the forward and reverse shock thermal X-rayemission from core-collapse and Type Ia supernova remnants (SNRs) which includethe efficient production of cosmic rays via non-linear diffusive shockacceleration (DSA). Our CR-hydro-NEI code takes into account non-equilibriumionization (NEI), hydrodynamic effects of efficient CR production on the SNRevolution, and collisional temperature equilibration among heavy ions andelectrons in both the shocked supernova (SN) ejecta and the shockedcircumstellar material. While X-ray emission is emphasized here, our codeself-consistently determines both thermal and non-thermal broadband emissionfrom radio to TeV energies. We include Doppler broadening of the spectral linesby thermal motions of the ions and by the remnant expansion. We study, ingeneral terms, the roles which the ambient environment, progenitor models,temperature equilibration, and processes related to DSA have on the thermal andnon-thermal spectra. The study of X-ray line emission from young SNRs is apowerful tool for determining specific SN elemental contributions, and forproviding critical information that helps to understand the type and energeticsof the explosion, the composition of the ambient medium in which the SNexploded, and the ionization and dynamics of the hot plasma in the shocked SNejecta and interstellar medium. With the approaching launch of thenext-generation X-ray satellite Astro-H, observations of spectral lines withunprecedented high resolution will become a reality. Our self-consistentcalculations of the X-ray spectra from various progenitors will help interpretfuture observations of SNRs.
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