E. Budding,
S. C. Marsden ,
O. B. Slee
, PASA, 18 (2), in press.
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Title/Abstract Page: The Active Algol Binary
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Conclusions
The ATCA light curves presented, covering slightly less than one complete orbital cycle at 4.848 and 4.976 GHz in one continuous run, show a definite level of emission at around 0.2-0.3 mJy above the background sky level. There is a slight indication of some real phase-dependent variation, but the low intensity data sample is also consistent with a more or less uniform level of emission with phase. Phase-related effects are supported by a small, but not very significant, correlation between the 4.848 and 4.976 GHz data sets. If real, there would be one main enhancement, rising in a quasi-symmetric manner to about 0.1 mJy above the background, over the phase range 0.5-0.9 and peaking at phase 0.7. The existence of the weak emission is suggestive of the gyrosynchrotron mechanism, as is often associated with RS CVn-like stars. However, the possibility of some separate emission effects peculiar to the Algol condition, and different to that of RS CVns, cannot be ruled out. This point calls for continued detailed studies of these classes of stellar radio source as data improves in quality and quantity.Next Section: Acknowledgements
Title/Abstract Page: The Active Algol Binary
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