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Infrared observations of Nova Cygni 1975
Ennis, D.; Becklin, E. E.; Beckwith, S.; Elias, J.; Gatley, I.; Matthews, K.; Neugebauer, G.; Willner, S. P.
AA(California Institute of Technology, Pasadena, Calif.), AB(California Institute of Technology, Pasadena, Calif.), AC(California Institute of Technology, Pasadena, Calif.), AD(California Institute of Technology, Pasadena, Calif.), AE(Hale Observatoires, Pasadena, Calif.), AF(Hale Observatoires, Pasadena, Calif.), AG(Hale Observatoires, Pasadena, Calif.), AH(Hale Observatoires, Pasadena, Calif.)
Astrophysical Journal, Part 1, vol. 214, June 1, 1977, p. 478-487. (ApJ Homepage)
Publication Date:
NASA/STI Keywords:
Infrared Astronomy, Novae, Stellar Envelopes, Stellar Spectrophotometry, Gas Expansion, Optical Thickness, Plasma Temperature, Stellar Evolution, Stellar Models, Thermal Emission
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Infrared photometry from 1 to 20 microns and spectroscopy at about 2 microns are presented for Nova Cygni 1975 for the period from 2 days before to 1 yr after maximum light. The data can be explained by a simple model in which the expanding gas expelled during the explosion is always a plasma at approximately 10,000 K. Initially the gas is optically thick; this phase clearly defines the time of onset of the nova. Later, as the gas continues to expand, it becomes optically thin. The temporal dependence of the observed flux suggests that in this phase the expanding cloud is in the form of a shell. After about 300 days, long-wavelength emission which may be attributable to thermal reradiation from dust is observed.

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