IUE observations of oxygen-rich supernova remnants

Details IUE observations of oxygen-rich supernova remnants IUE observations of oxygen-rich supernova remnants

Jun 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988esasp.281a.117b&link_type=abstract

In ESA, A Decade of UV Astronomy with the IUE Satellite, Volume 1 p 117-120 (SEE N89-10682 01-89)

Astronomy and Astrophysics

Astronomy

4

Iue, Magellanic Clouds, Oxygen Spectra, Spaceborne Astronomy, Supernova Remnants, Ultraviolet Astronomy, Abundance, Astronomical Models, Nuclear Fusion

Scientific paper

The IUE observations were used to determine the composition of the ejecta (especially C and Si abundances) and to test models for the ionization and excitation of the ejecta of two oxygen-rich supernova remnants (N132D in the Large Magellanic Cloud and 1E 0102-7219 in the Small Magellanic Cloud). Time-dependent photoionization by the EUV and X-ray radiation from 1E 0102-7219 can qualitatively explain its UV and optical line emission, but the density and ionization structures are complex and prevent a unique model from being specified. Many model parameters are poorly constrained, including the time dependence and shape of the ionizing spectrum. Moreover, the models presented are not self-consistent in that the volumes and densities of the optically emitting gas imply optical depths of order unity in the EUV, but absorption of the ionizing radiation was ignored. It is possible that these shortcomings reflect a more fundamental limitation of the model assumptions. It is assumed that the electron velocity distribution is Maxwellian and that the energy deposited by photoionization heats the electrons directly. The 500 eV electrons produced by the Auger process may excite or ionize other ions before they slow down enough to share their energy with other electrons. Many of the excitations would produce photons that could ionize lower ionization stages.

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