Astronomy and Astrophysics – Astronomy
Scientific paper
May 1980
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980apj...237..769s&link_type=abstract
Astrophysical Journal, Part 1, vol. 237, May 1, 1980, p. 769-780.
Astronomy and Astrophysics
Astronomy
104
Infrared Astronomy, Interstellar Gas, Molecular Gases, Nebulae, Stellar Evolution, Supernova Remnants, Gas Ionization, Gas Temperature, Infrared Spectra, O Stars, Signature Analysis, Stellar Luminosity, Stellar Temperature
Scientific paper
The structure and emission of a supernova remnant embedded in a dense molecular cloud are studied. During the early life of the remnant, grain emission from the interior produces an infrared maximum. At later stages, the X-rays from the hot interior create a region of warm, partially ionized gas outside the shell, in which most of the luminosity is reprocessed by grains into far-infrared radiation. The pulsar left as a remnant of the explosion can deposit an energy comparable to the initial explosion in a time that is short compared to the shell-formation time +(sq). For an ambient density of 100,000/cu cm, the initial infrared flash of 2.5 x 10 to the 8th solar luminosities is followed by a secondary luminosity peak of 10-million solar luminosities after a time +(sq) = 20 yr and fades thereafter as (+/+/sq/) exp -8/7. A sizable number of buried supernovae could resolve the apparent discrepancy between pulsar and supernova birthrates.
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