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Imaging and Spectroscopy of Abell 63 (UU SGE)

Published online by Cambridge University Press:  07 August 2017

N.A. Walton ,
J.R. Walsh  and
S.R. Pottasch
N.A. Walton
Affiliation:
Department of Physics & Astronomy, University College London, Gower Street, London WC1E 6BT, England
J.R. Walsh
Affiliation:
Space Telescope European Coordinating Facility, European Southern Observatory, Karl-Schwarzschild-Strasse 2, D8046 Garching bei München, Germany
S.R. Pottasch
Affiliation:
Kapteyn Laboratorium, Rijksuniversiteit Groningen, Postbus 800, 9700 AV Groningen, The Netherlands

Abstract

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UU Sge, the eclipsing binary central star (Bond et al, 1978) of the low-surface-brightness planetary nebula (PN) Abell 63, has been observed spectroscopically in the visible throughout its 11.2 hour period and especially during the minimum. A spectral determination of the binary system has been made. The primary hot central star is an ‘O’ type PN nucleus of temperature ≈40,000 K, consistent with the low excitation of the nebular spectrum (e.g. no He ii 4686Å nebular emission detected). From the spectrum at minimum light, the secondary star appears to be a cool dwarf star around G7. Measurement of the magnitude of the secondary during the eclipse of the primary enabled the distance to the PN to be directly determined as 3.6 kpc. For this distance the luminosity of the hot star is approximately 4 320 L⊙, in good agreement with evolutionary tracks for (single) PN nuclei. Deep CCD images of Abell 63 show it has a ‘butterfly’ morphology implying that the close binary central system may have had a strong effect on the nebula shaping. The paper describing this work has been submitted (Walton et al, 1992).

Type
IV. Planetary Nebulae Connection: Evolution from the AGB
Information
Symposium - International Astronomical Union , Volume 155: Planetary Nebulae , 1993 , pp. 394
Copyright
Copyright © Kluwer 1993 

References

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