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The Orbital Period of Nova V2540 Ophiuchi (2002)

Published online by Cambridge University Press:  05 March 2013

Tansel Ak ,
Alon Retter  and
Alex Liu
Tansel Ak*
Affiliation:
Department of Astronomy and Space Sciences, Faculty of Science, Istanbul University, 34119 University, Istanbul, Turkey
Alon Retter
Affiliation:
Department of Astronomy and Astrophysics, Pennsylvania State University, University Park, PA 16802-6305, USA
Alex Liu
Affiliation:
Norcape Observatory, PO Box 300, Exmouth WA 6707, Australia
*
DCorresponding author. Email: tanselak@instanbul.edu.tr
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Abstract

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We present the results of 26 nights of CCD photometry of the nova V2540 Oph (2002) from 2003 to 2004. We find a period of 0.284781 ± 0.000006 d (6.8347 ± 0.0001 h) in the data. Since this period was present in the light curves taken in both years, with no apparent change in its value or amplitude, we interpret it as the orbital period of the nova binary system. The mass–period relation for cataclysmic variables yields a secondary mass of about 0.75 ± 0.04 M⊙. From maximum magnitude–rate of decline relation, we estimate a maximum absolute visual magnitude of MV = −6.2 ± 0.4 mag. This value leads to an uncorrected distance modulus of (m – M) = 14.7 ± 0.7. By using the interstellar reddening for the location of V2540 Oph, we find a rough estimate for the distance of 5.2 ± 0.8 kpc. We propose that V2540 Oph is either (1) a high-inclination cataclysmic variable showing a reflection effect of the secondary star, or having a spiral structure in the accretion disc, (2) a high-inclination intermediate polar system, or less likely (3) a polar.

Keywords

accretion, accretion discsstars: individual: V2540 Oph, novae, cataclysmic variables
Type
Research Article
Information
Publications of the Astronomical Society of Australia , Volume 22 , Issue 4 , 2005 , pp. 298 - 305
Copyright
Copyright © Astronomical Society of Australia 2005

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