Time development of the near-infrared spectrum of the slow nova V2214 Ophiuchi (Nova Ophiuchi 1988)

Details Time development of the near-infrared spectrum of the slow nova V2214 Ophiuchi (Nova Ophiuchi 1988) Time development of the near-infrared spectrum of the slow nova V2214 Ophiuchi (Nova Ophiuchi 1988)

Jun 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aj....103.1970e&link_type=abstract

Astronomical Journal (ISSN 0004-6256), vol. 103, no. 6, June 1992, p. 1970-1975. Research supported by Aerospace Corp.

Other

5

Near Infrared Radiation, Novae, Stellar Evolution, Stellar Spectra, Emission Spectra, Helium, Line Spectra, Stellar Coronas, Stellar Spectrophotometry

Scientific paper

Spectrophotometric observations are presented from 0.9 to 1.3 microns of the classical nova V2214 Ophiuchi (Nova Ophiuchi 1988) obtained in July 1989. V2214 Oph was a slow nova, with t3 = about 220 days. The spectrum displays a weak continuum with emission lines of hydrogen, He I 10830, He II, and forbidden N I. When compared to the September 1988 spectrum reported by Lynch et al. (1989), the strength of the continuum and the emission lines are found to have declined by roughly a factor of 10, with the exception of the He II lines, which were very weak in the earlier spectrum but are prominent in the 1989 data. The strength of the He II features suggest that the nova had entered its early nebular phase. The concurrence of infrared coronal and He II lines in this and several other novae suggests that photoionization, rather than collisional ionization by shock heating, may be the predominant mechanism for generating the parent species of IR coronal lines.

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