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The Oxygen 1.13 μm Fluorescence Line of SN1987A: a Diagnostic for the Ejecta of Hydrogen-Rich Supernovae

Published online by Cambridge University Press:  12 April 2016

Ernesto Oliva
Ernesto Oliva*
Affiliation:
Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 1-50125 Firenze, Italy

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The bright O I λ11287 line observed in SN1987A is produced by the Bowen fluorescence with Lyβ and comes from regions that lie within a Sobolev length (δR ∼ 10-3RSN, the maximum distance over which fluorescence can work) from hydrogen rich gas ionized by the 56Co decay. Its strength relative to hydrogen lines (e.g. Brγ) depends on the O/H relative abundance in the ‘fluorescent region’ and on the density (i.e. the filling factor) of the gas. The observed evolution of λ11287 can be successfully understood using a relatively simple theory which takes into account the effects of transfer in the O I lines and is the generalization of the classical theory of Bowen fluorescence.

Type
SN 1987A, SN 1993J, and Other Supernovae
Information
International Astronomical Union Colloquium , Volume 145: Supernovae and Supernova Remnants , 1996 , pp. 235 - 240
Copyright
Copyright © Cambridge University Press 1996

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