Research Articles

Modelling of W UMa-type variable stars

P. L. Skelton, D. P. Smits
South African Journal of Science | Vol 105, No 3/4 | a62 | DOI: https://doi.org/10.4102/sajs.v105i3/4.62 | © 2010 P. L. Skelton, D. P. Smits | This work is licensed under CC Attribution 4.0
Submitted: 19 January 2010 | Published: 19 January 2010

About the author(s)

P. L. Skelton, Department of Mathematical Sciences, P.O. Box 392, UNISA 0003, South Africa., South Africa
D. P. Smits, Department of Mathematical Sciences, P.O. Box 392, UNISA 0003, South Africa., South Africa

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Abstract

W Ursae Majoris (W UMa)-type variable stars are over-contact eclipsing binary stars. To understand how these systems form and evolve requires observations spanning many years, followed by detailed models of as many of them as possible. The All Sky Automated Survey (ASAS) has an extensive database of these stars. Using the ASAS V band photometric data, models of W UMatype stars are being created to determine the parameters of these stars. This paper discusses the classification of eclipsing binary stars, the methods used to model them as well as the results of the modelling of ASAS 120036–3915.6, an over-contact eclipsing binary star that appears to be changing its period.

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