Volume 366, Number 3, February II 2001
|Page(s)||858 - 864|
|Section||Interstellar and circumstellar matter|
|Published online||15 February 2001|
The 2000 outburst of the recurrent nova CI Aquilae: Optical spectroscopy*
Department of Experimental Physics and Astronomical Observatory, University of Szeged, Dóm tér 9., Szeged 6720, Hungary
2 Guest Observer at Konkoly Observatory
3 University of Toronto, David Dunlap Observatory, Richmond Hill, Canada
4 Mt. Suhora Observatory of the Pedagogical University, Cracow, Poland
Corresponding author: L. L. Kiss, firstname.lastname@example.org
Accepted: 13 November 2000
We present low- and medium resolution spectra of the recurrent nova CI Aquilae taken at 14 epochs in May and June, 2000. The overall appearance is similar to other U Sco-type recurrent novae (U Sco, V394 CrA). Medium resolution (-) hydrogen and iron profiles suggest an early expansion velocity of 2000-2500 km s-1. The Hα evolution is followed from = -0.6 d to +53 d, starting from a nearly Gaussian shape to a double peaked profile through strong P-Cyg profiles. The interstellar component of the sodium D line and two diffuse interstellar bands put constraints on the interstellar reddening which is estimated to be =. The available visual and CCD-V observations are used to determine t0, t2 and t3. The resulting parameters are: , d, d. The recent lightcurve is found to be generally similar to that observed in 1917 with departures as large as 1-2 mag in certain phases. This behaviour is also typical for the U Sco subclass.
Key words: stars: novae / stars: individual: CI Aql
© ESO, 2001
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.