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Surface Imaging of Late-Type Contact Binaries II: Hα Emission in AE Phe and YY Eri

Published online by Cambridge University Press:  09 August 2007

O. Vilhu
Affiliation:
Observatory, Box 14, FIN-00014 University of Helsinki, Finland email: osmi.vilhu@helsinki.fi
C. Maceroni
Affiliation:
INAF, Osservatorio Astronomico di Roma, via Frascati 33, I-00040 Monteporzio (RM)Italy email: maceroni@oa-roma.inaf.it
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Abstract

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We present and discuss the Hα (λ = 6563Å) observations of the contact (W UMa type) binaries AE Phoenicis and YY Eridani, obtained in 1989, 1990 and 1995 with the CAT/CES telescope of the Southern European Observatory (ESO). In particular, we compare the intrinsic equivalent widths of both components with the NextGen theoretical models and the saturation limit. We find that the average Hα equivalent widths are close to the saturation border and that the primary components have excess Hα-emission, indicating enhanced chromospheric activity. This is compatible with both theoretical and observational suggestions that the primary is the more magnetically active component and is filled with (mostly unresolvable) dark spots and associated chromospheric plages.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2007

Footnotes

based on observations collected at the European Southern Observatory, La Silla, Chile

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