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Orbital Parameters of the Close Binary Central Stars of NGC 6337 and NGC 6026

Published online by Cambridge University Press:  15 December 2006

Todd C. Hillwig ,
Howard E. Bond  and
Melike Afsar
Todd C. Hillwig
Affiliation:
Department of Physics and Astronomy, Valparaiso University, Valparaiso, IN 46383, USA email: todd.hillwig@valpo.edu
Howard E. Bond
Affiliation:
Space Telescope Science Institute
Melike Afsar
Affiliation:
Ege University, Turkey
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Abstract

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We present the results of time-resolved photometry and spectroscopy of the central star of the planetary nebula NGC 6026 and time-resolved photometry of the central star of the planetary nebula NGC 6337. The results of period analysis give an orbital period of 0.528088 days for NGC 6026 and a photometric period of 0.173474 days for NGC 6337. In the case of NGC 6337 it appears that the photometric period accurately reflects the orbital period and that the variability is the result of an irradiated hemisphere on the cool companion. For NGC 6026 however, radial velocities from spectroscopy show that the orbital period is twice the photometric period. In this case, the photometric variability is due to an ellipsoidal effect in which one of the stars fills, or nearly fills, its Roche lobe. Based on the data and modeling using the Wilson-Devinney code, we discuss the physical parameters of the two systems. We also relate the physical parameters to the shape and orientation of the nebulosity.

Keywords

binaries: closeplanetary nebulae: individual (NGC 6337, NGC 6026)subdwarfswhite dwarfs
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S234: Planetary Nebulae in our Galaxy and Beyond , April 2006 , pp. 421 - 422
Copyright
© 2006 International Astronomical Union