The reionization of unshocked ejecta in SN 1006

Details The reionization of unshocked ejecta in SN 1006 The reionization of unshocked ejecta in SN 1006

Apr 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988apj...327..178h&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 327, April 1, 1988, p. 178-196.

Astronomy and Astrophysics

Astronomy

50

Shock Waves, Stellar Coronas, Supernova Remnants, Ultraviolet Astronomy, Ultraviolet Spectra, White Dwarf Stars, Absorption Spectra, Astronomical Models, Iue, Photoionization, Radiative Transfer, Time Dependence

Scientific paper

The validity of carbon-deflagration models white dwarf models for type Ia supernovae is investigated by examining whether most of the iron in the center of SN 1006 exists in forms other than Fe II, such as iron grains or other ionic stages of iron, as the models require. The possible ways in which iron can be hidden in SN 1006 are reviewed, and an argument on observational grounds is made against any appreciable fraction of iron in grains or Fe I. Various mechanisms for ionizing unshocked iron beyond Fe II are discussed; the most probable mechanism for ionizing the iron appears to be photoionization by UV and X-ray emission from reverse-shocked ejecta. A detailed model for this reverse-shcok photoionization mechanism is described.

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