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Astron. Astrophys. 315, L209-L212 (1996)

ISO observations of the classical nova V1974 Cygni*

A. Salama1, A. Evans2, S.P.S. Eyres2, K. Leech1, P. Barr1, and M.F. Kessler1

1 ISO Science Operations Centre, Astrophysics Division of ESA, Postbox 50727, E-28080 Villafranca/Madrid, Spain
2 Department of Physics, Keele University, Keele, Staffordshire, ST5 5BG, UK

Received 16 July 1996 / Accepted 20 August 1996

Abstract. We present observations of the classical nova V1974 Cygni (Nova Cyg 1992) obtained with the ISO Short and Long Wavelength Spectrometers (SWS and LWS) and the spectrometer section of ISOPHOT. We identify [NeIII] img3.gif15.5, [NeV] img3.gif14.3, 24.3, [NeVI] img3.gif7.6, [OIII] img3.gif51.8, [OIV] img3.gif25.9. There is evidence that the Ne and O emission arises in physically distinct regions of the ejecta. We determine the electron temperatures in the Ne- and O-bearing regions of the ejecta, and estimate the Ne abundance relative to O.

Key words: circumstellar matter - stars: individual: V1974 Cyg - novae, cataclysmic variables - infrared: stars

* The Infrared Space Observatory (ISO) is an ESA project with instruments funded by ESA Member States (especially the PI countries: France, Germany, the Netherlands and the United Kingdom) and with the participation of ISAS and NASA

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