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Further Discussion of Binary Star Radio Survey Data

Published online by Cambridge University Press:  05 March 2013

E. Budding ,
O. B. Slee  and
K. Jones
E. Budding
Affiliation:
Central Institute of Technology, PO Box 40740, Upper Hutt, Wellington, New Zealand Carter Observatory, PO Box 2909, Wellington, New Zealand; Edwin.Budding@cit.ac.nz
O. B. Slee
Affiliation:
Australia Telescope National Facility, PO Box 76, Epping, NSW 2121, Australia; bslee@atnf.csiro.au
K. Jones
Affiliation:
Physics Department, University of Queensland, St Lucia, Qld 4072, Australia; jones@physics.uq.oz.au
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Abstract

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Statistical information on 8280 individual radio observations of binary stars, predominantly at 8·4 GHz using the Parkes 64 m antenna, is presented. Three main groups are distinguished: (i) RS CVn stars, (ii) classical Algol binaries (EA2s), and (iii) detached pairs of generally early type (ETBs).

The RS CVn stars more frequently gave rise to detectable fluxes, while the ETBs, in these data, are a small and rather heterogeneous class. The Algols' emission appears to increase near conjunction phases, though we cannot clearly distinguish any special property of the Algols' phase-dependent behaviour that is not also shared by the RS CVn binaries. Both these categories' data show a bimodal, phase-dependent pattern to the distribution of detections, suggesting that these binary types share similar underlying physical properties, though there could also be other factors at play. The sample sizes of the Algols and particularly the ETB detections are too small for effective, discriminatory statistics, however.

Keywords

binary starsRS CVnsAlgolsradio emission
Type
Research Article
Information
Publications of the Astronomical Society of Australia , Volume 15 , Issue 2 , 1998 , pp. 183 - 188
Copyright
Copyright © Astronomical Society of Australia 1998

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