The evolution of the 8-13 micron spectrum of supernova 1987A

Details The evolution of the 8-13 micron spectrum of supernova 1987A The evolution of the 8-13 micron spectrum of supernova 1987A

Apr 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993mnras.261..522r&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 261, no. 3, p. 522-534.

Astronomy and Astrophysics

Astronomy

32

Infrared Spectra, Interstellar Extinction, Supernova 1987A, Astronomical Spectroscopy, Infrared Stars

Scientific paper

The study presents spectra at 8-13 microns of SN 1987A, obtained on 12 dates between days 54 and 850 after the explosion. Fine-structure lines of heavy elements, which dominated the spectrum between days 300 and 550, are analyzed to derive masses of cobalt and chlorine which are in good agreement with model predictions. An upper limit to the ratio of Co-57 to Co-56 of 1.6 times the solar Fe-57-to-Fe-56 ratio is derived, which is also in good agreement with models, but precludes the possibility that enhanced Co-57 could account for a high bolometric luminosity at late times. The ionization balance of the heavy elements shifted from greater than about 90 percent singly ionized at the end of the first year to greater than about 50 percent neutral by day 600. It is inferred that the dust emission was optically thin and that some of the emitting trains must have subtended an angle larger than that defined by the ejecta traveling at 2000 km/s. It is argued that the bulk of the dust must have formed in the ejecta, and that at most only a small fraction of the mid-IR emission could have arisen from an IR echo.

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