Astronomy and Astrophysics – Astrophysics
Scientific paper
Oct 1995
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995ap%26ss.232..355b&link_type=abstract
Astrophysics and Space Science, Volume 232, Issue 2, pp.355-376
Astronomy and Astrophysics
Astrophysics
13
Scientific paper
Photometry of the southern RS CVn binary CF Tuc collected from over a sixteen year period since December 1978, is analysed. 25 data-sets, mainly in broadbandV, have been studied for trends in the effects of surface maculation. The data-sets were divided into four intervals of more continuous records. From these we find the following: (a) Maculation tends to concentrate in certain restricted regions of longitude, so that distinct ‘waves’ can often be seen. These maculation waves can be modelled with one or two large circular dark regions - ‘starspots’, plausibly at higher latitudes, in comparison with the familiar solar case. (b) Such a spot often prefers a longitude close to, but frequently a little before, that of the central meridian at primary minimum. A latitude of ~ ±(40-50) deg is feasible at this stage. (c) From this position the spot will tend to drift to lower phases over the timescale of a year or so, and at a rate of typically 30 50 deg/year. (d) There are indications that such a spot will drift downward in latitude during this process. (e) After a given large spot has drifted back to the phase of near second quadrature, a new formation will typically start to appear around the primary conjunction phase. (f) At, or a little after, this stage, the maculation effects can become quite complex, without a small number of predominating features. (g) A near-conjunction feature will subsequently tend to predominate as at (b). We tentatively posit an activity ‘cycle’ (b) → (f) → (b) taking typically around five to six years. More continuous and detailed photometric monitoring could help substantiate or improve on this picture, thus augmenting our knowledge of stellar magnetodynamic activity.
Budding Edwin
Zeilik Michael
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