Theoretical studies of X-ray emission from supernova remnants and other non-equilibrium astrophysical plasmas

Details Theoretical studies of X-ray emission from supernova remnants and other non-equilibrium astrophysical plasmas Theoretical studies of X-ray emission from supernova remnants and other non-equilibrium astrophysical plasmas

Mar 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984sao..rept.....d&link_type=abstract

Final Report, 1 Nov. 1980 - 29 Feb. 1984 Smithsonian Astrophysical Observatory, Cambridge, MA.

Statistics

Computation

Computer Programs, Computerized Simulation, Dielectric Properties, Electron Flux Density, Iron, Nonequilibrium Plasmas, O Stars, Space Plasmas, Stellar Winds, Supernova Remnants, X Ray Sources, X Ray Spectroscopy, Atomic Excitations, Atomic Spectra, Electron Orbitals, Electron Photon Cascades, Electron States, Ion Production Rates, Ion Recombination, Light Emission, Plasma-Particle Interactions, Ultraviolet Spectroscopy

Scientific paper

To improve the accuracy of thermal X-ray emission spectrum predictions, new computations of electron excitation rates, dielectric recombination rates, and updated codes were applied to existing data on supernova remnants and O star winds. Because of its general predominance along with low ionization and recombination rates, Fe(XVII) was analyzed with the inclusion of resonances to the excitation rate data. Corrections to the existing dielectric recombination rates based on detailed Fe (XVII) calculations and the more approximate Quantum Defect Method were accomplished. by using Distorted Wave ionization rates and reliable excitation rates, models for X-ray, ultraviolet, and optical emission line intensities of non-radiative shock wave can be constructed that supply data on shock velocity, preshock ionization states, and elemental abundances. The radiative driving force that drives the shock wave is calculated through line opacities of the shocked gas. X-ray emission spectra are also calculated for O star winds.

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