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E. Behar, A. Rasmussen, J. Cottam, S.M. Kahn, F.B.S. Paerels, J.R. Peterson, M. Sako (Columbia Astophysics Laboratory, Columbia University), A.C. Brinkman, A.J.F. den Boggende, J.W. den Herder, C.P. de Vries, C. Ferrigno, J.S. Kaastra, R. Mewe, T. Tamura, K.J. van der Heyden (Space Research Organization of the Netherlands), G. Branduardi-Raymont, I. Sakelliou (Mullard Space Science Laboratory, University College London), M. Audard, M. Gudel (Paul Scherrer Institiute), C. Erd (Space Science Department, European Space Agency)
Shocked plasmas of young supernova remnants (SNRs) are in a transient (but very long) phase of being ionized. In these remnants, the temperature is high compared with the charge states present in the plasma. Consequently, the standard single-ion collisional plasma models are inadequate for analyzing SNR spectra. We have developed a non equilibrium ionization model that includes two or more successive charge states. All of the spontaneous and electron-impact atomic processes are incorporated in the model, including radiative recombination, autoionization, and inner-shell ionization, some of which can be of vast importance in SNR plasmas. Based on the HULLAC atomic code, the model is highly versatile and can basically run for any desired highly ionized species. Synthetic spectra are calculated for various plasma conditions and compared with RGS spectra of several SNRs in the Magellanic Clouds, namely 1E0102-72.3, N132D, N49, and 0519-69.0.
The author(s) of this abstract have provided an email address for comments about the abstract: behar@astro.columbia.edu