Computer Science
Scientific paper
Aug 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003phdt.........8h&link_type=abstract
Thesis (PhD). NORTH CAROLINA STATE UNIVERSITY, Source DAI-B 64/02, p. 763, Aug 2003, 176 pages.
Computer Science
2
Scientific paper
The study of supernovae and the expanding remnants that form after the explosion is important to understanding star formation and the distribution of elements in the interstellar medium (ISM). This work examines the X-ray spectrum of 14 LMC remnants: three new Chandra observations, and eleven archival ASCA observations. The plasma that is responsible for the X-ray emission is heated by a shock wave created by the supernova explosion that expands into the ISM. The picture is further complicated by a reverse shock that is created at the interface between the ISM and the material ejected from the star by the explosion. Non-equilibrium ionization (NEI) models are used to describe the thermal contributions to the spectrum. Existing models assume that hydrogen and helium are the sole source of electrons in the plasma. A new NEI model is introduced and tested which accounts for the overabundance of heavy elements in the remnant ejecta and their contribution to the electron density. This is a plane-parallel shock model that can account for non- Coulomb heating at the shock front and uses shock velocity as a parameter rather than shock temperature. Hard, non-thermal tails that are well described by a power law have been observed in the X-ray spectra of several remnants. Synchrotron radiation observed in the radio regime for low energy electrons can be extrapolated to X-ray energies to account for high energy (>1 TeV) electrons. By combining X-ray data with radio observation parameters we can constrain the maximum energies of the shock-accelerated electrons in the supernovae. None of the remnants in this study have a maximum energy above 100 TeV. SNR 0534-69.9 and SNR 0548-70.4 spectra show middle-aged remnants with significant contributions from the ejecta inside the outer shell. The ejecta detection allowed the classification of a Type Ia progenitor for both. The SNR 0453-68.5 observation indicates a core- collapse explosion due to the presence of a pulsar wind nebula.
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