[Previous] | [Session 57] | [Next]
R. Ignace (University of Iowa), M.A. Hendry (University of Glasgow, Scotland, UK)
We have derived a method for inverting emission line profiles formed in supernova ejecta. The derivation assumes spherical symmetry and homologous expansion (i.e., v(r) \propto r). The inversion is analytic and even takes account of occultation by a pseudo-photosphere. Previous inversion methods have been developed which are restricted to optically thin lines, but the particular case of homologous expansion permits an analytic inversion for lines of arbitrary optical depth. In fact, we show that the quantity that is generically retrieved is the run of line intensity I\lambda with radius in the ejecta shell. This result could be applied to resonance lines, recombination lines, or lines dominated by collisional de-excitation.
The author(s) of this abstract have provided an email address for comments about the abstract: ri@astro.physics.uiowa.edu