Near-Infrared Emission Lines of V723 Cassiopeiae (Nova Cassiopeiae 1995)

Details Near-Infrared Emission Lines of V723 Cassiopeiae (Nova Cassiopeiae 1995) Near-Infrared Emission Lines of V723 Cassiopeiae (Nova Cassiopeiae 1995)

Jul 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002apj...573..794r&link_type=abstract

The Astrophysical Journal, Volume 573, Issue 2, pp. 794-802.

Astronomy and Astrophysics

Astronomy

15

Infrared: Stars, Line: Identification, Stars: Novae, Cataclysmic Variables, Stars: Individual: Constellation Name: V723 Cassiopeiae

Scientific paper

Near-infrared spectroscopy (0.8-2.5 μm) from two epochs is presented for the very slow nova V723 Cassiopeiae (=Nova Cassiopeiae 1995). Its bright, comparatively narrow emission lines (FWHM~500 km s-1) make it ideal for determining wavelengths of unidentified emission lines that appear in the nebular/coronal stages of novae. We present wavelengths for 16 previously unobserved or unidentified features and search for identifications by looking for coincidences with known atomic transitions. For a candidate transition, the likely abundance of the parent ion is considered and then a collisional, fluorescent, or recombination process capable of exciting the feature is sought. Four of the lines are identified in this manner, all of them collisionally excited, forbidden transitions. One of these, [Ti VII] λ22050, is a new coronal line that de-excites directly to the ground state. Three other lines are associated with transitions from collisionally excited, low-lying, metastable levels of Fe+5. Of the remaining unidentified features, five, with wavelengths of 8926, 11110, 11900, 15545, and 20996 Å, have been observed in other novae. Comparing the time development of these features with the [S VIII] λ9913 coronal line indicates that all have parent ions of lower excitation (<280 eV) than S+7.

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