Late emission from SN 1987A

Details Late emission from SN 1987A Late emission from SN 1987A

Nov 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987apj...322l..15f&link_type=abstract

Astrophysical Journal, Part 2 - Letters to the Editor (ISSN 0004-637X), vol. 322, Nov. 1, 1987, p. L15-L20.

Astronomy and Astrophysics

Astrophysics

62

Emission Spectra, Stellar Evolution, Stellar Mass Ejection, Stellar Spectrophotometry, Supernovae, Cosmic Gases, Infrared Spectra, Pulsars, Stellar Models, Visible Spectrum

Scientific paper

Assuming that the progenitor star of SN 1987A had an initial mass in the 15 - 25 M_sun; range and had undergone considerable mass loss, the authors model the late emission from the mantle gas under the assumption of energy input by γ-rays from 56Co decays. An emission-line spectrum of low-ionization species is produced at optical through infrared wavelengths. At an age of ≡700 days an infrared catastrophe occurs and the gas temperature drops to a few hundred K; most of the radiation is then emitted in infrared fine-structure lines. The γ-ray line intensity peaks in the 15 M_sun; model at an age of 270 days. Radiation from a possible central pulsar nebula will be absorbed by the mantle gas; optical depth unity in the 15 M_sun; model at 10 keV is not reached for 18 yr. The radio emission from the pulsar is likely to be absorbed by the ejecta for several years.

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