EDP Sciences
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Volume 448, Number 3, March IV 2006
Page(s) 1107 - 1110
Section Stellar structure and evolution
DOI http://dx.doi.org/10.1051/0004-6361:20047022
A&A 448, 1107-1110 (2006)
DOI: 10.1051/0004-6361:20047022

The possible orbital period of the nova V1493 Aquilae

A. Dobrotka1, M. Friedjung2, A. Retter3, 4, L. Hric5 and R. Novak6

1  Departement of Physics, Faculty of Materials Science and Technology, Slovak University of Technology in Bratislava, Paulínska 16, 91724 Trnava, The Slovak Republic
    e-mail: andrej.dobrotka@stuba.sk
2  Institut d'Astrophysique de Paris, 98 bis boulevard Arago, 75014 Paris, France
    e-mail: fried@iap.fr
3  Departement of Astronomy and Astrophysics, Penn State University, 525 Davey Lab, University Park, PA, 16802-6305, USA
    e-mail: retter@astro.psu.edu
4  School of Physics, University of Sydney, 2006, Australia
5  Astronomical Institute of the Slovak Academy of Sciences, 05960 Tatranská Lomnica, The Slovak Republic
    e-mail: hric@ta3.sk
6  Nicholas Copernicus Observatory and Planetarium in Brno, Kraví Hora 2, 61600 Brno, Czech Republic
    e-mail: novak@hvezdarna.cz

(Received 7 January 2004 / Accepted 8 November 2005)

Aims.Period analysis of CCD photometry of V1493 Aql (Nova Aql 1999 No. 1) performed during 12 nights through I and R filters a few weeks after maximum is presented.
Methods.The PDM method for period analysis (Stellingwerf 1978, ApJ, 224, 953) is used.
Results.The photometric data is modulated with a period of $0.156 \pm 0.001$ d. Following the sinusoidal shape of the phased light curve, we interpret this periodicity as possibly orbital in nature and that is consistent with a cataclysmic variable above the period gap.

Key words: binaries: close -- binaries: eclipsing -- novae, cataclysmic variable

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