Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993aas...183.3806c&link_type=abstract
American Astronomical Society, 183rd AAS Meeting, #38.06; Bulletin of the American Astronomical Society, Vol. 25, p.1348
Astronomy and Astrophysics
Astronomy
Scientific paper
The observations of CO and SiO in the infrared spectrum of SN1987A clearly indicate that molecules can form in the debris of a supernova explosion. Since H_2 is not easily observable we compute its abundance theoretically. For conditions typical of the inner (v < 2500 km s(-1) ) envelope of SN1987A, the fraction of H that is in molecular form rises to ~ 1% by t ~ 800 d. For t < 500 d the formation is dominated by the gas phase reactions H + H(+) -> H_2(+) + h nu ; H_2(+) + H -> H_2 + H(+) . Thereafter, the formation is dominated by the reactions H + e -> H(-) + h nu ; H(-) + H -> H_2 + e. At early times the H(-) may absorb ~ 10-30% of visible photons, contributing to the apparent paucity of H alpha emission. For t > 800 d the abundance of H_2 ``freezes out'' due to the slowing of all reactions. The opacity of the supernova envelope in the range 912 < lambda < 1150 Angstroms is dominated by resonance scattering in the Lyman and Werner bands of H_2. The resulting fluorescence emission bands of H_2 in the range 1150 < lambda < 1650 Angstroms may be observable in the UV spectra of supernovae at late times.
Culhane Michael
McCray Richard
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