Simulations of Supernova Remnants in Diffuse Media. II. Three Remnants and Their X-Ray Emission

This paper provides detailed descriptions of the X-ray emission from supernova remnants evolving in warm, low density, nonthermal pressure dominated regions (To = 10 4 K, n = 0.001 cm, Pnt = 1800 or 7200 K cm ). Non-equilibrium ionization hydrocode simulations are used to predict the high resolution spectra, 1/4 and 3/4 keV ROSAT PSPC countrates, spatial appearance, color temperatures, and ratios of O VII to O VIII emission line fluxes as a function of time. If undisturbed, the remnants are quite long lived, surviving for ∼ 1.2 to ∼ 1.6×10 yrs. During their brief energy conserving phases, the hot, highly pressurized gas behind their shock fronts copiously emit X-rays. Thus, their 1/4 keV surface brightnesses are thousands of ROSAT PSPC counts s arcmin and the remnants appear strongly edge brightened. The onset of the radiative phase heralds the end of the extreme X-ray luminosities, but not the end of the X-ray emission. After the cool shell forms behind the shock front, the hot SNR bubble slowly radiates away the remaining energy, with a diminutive fraction released in the form of X-rays. Thus, the 1/4 keV surface brightnesses are tens to hundreds of ROSAT PSPC counts s arcmin and the remnants appear “centrally filled”. The hot plasma within the remnant bubbles is always out of collisional ionizational equilibrium. Early on, the ionization states are much lower than expected for such hot gas. Later on, the ionization states are higher. This paper also applies the standard observational analyses for determining the color