Time Development of Recurrent Nova CI Aquilae's 2000 Outburst between 0.8 and 2.5 MICRONS

Details Time Development of Recurrent Nova CI Aquilae's 2000 Outburst between 0.8 and 2.5 MICRONS Time Development of Recurrent Nova CI Aquilae's 2000 Outburst between 0.8 and 2.5 MICRONS

Feb 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aj....127.1089l&link_type=abstract

The Astronomical Journal, Volume 127, Issue 2, pp. 1089-1097.

Astronomy and Astrophysics

Astronomy

11

Infrared Radiation, Stars: Novae, Cataclysmic Variables, Stars: Individual (Ci Aquilae)

Scientific paper

We report 0.8-2.5 μm spectrophotometry of CI Aquilae at eight epochs between 2000 May 9 and 2001 June 2 UT, corresponding to approximately 3 and 391 days after peak brightness. Near peak brightness, the spectra showed emission lines that were characteristic of a low-excitation, nitrogen-rich shell. Within a few weeks, the spectra began to show higher excitation/ionization emission lines indicative of a harder illuminating source: the neutral metal lines faded, leaving only lines of H I, He I, and He II and the emerging coronal lines. A month after peak brightness, the [Ca VIII] coronal line at 2.3205 μm appeared and persisted until the last of our observations, on day +391. From the O I line ratios, we deduced a reddening of EB-V=1.5+/-0.1 and a visual extinction of AV=4.6+/-0.2. Along with the rate of decline from the light curve (t2), we derived a distance of 2.6+/-1.3 kpc. The frequently observed unidentified novae lines were present in CI Aquilae along with a potentially new member of the group at 2.425+/-0.002 μm.

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